HISTORY AND WORK OF The Warmer Observatory, rochester, h. y. 1883-1886. VOL. I. The original of tiiis book is in tine Cornell University Library. There are no known copyright restrictions in the United States on the use of the text. http://www.archive.org/details/cu31924031362001 ADDBNDA. The number of nebulce discovered at tlie Warner Ohservatory up to Jan. 1, 1887. rejecting tliose reserved for veriilcation and further examination, is 540. The work of the current year will be not only a continuation of that pursued during the past three years, but also the study of such of those nebula; found by former discoverers, as shall present themselves in the quest for new ones, which shall seem to possess sufficient atti'activeness to warrant the necessary outlay of time. Since the list of the Warner prizes was electrotyped, the following comet prizes have been paid: DATE. DISCOVEEEK. AM'T OF PRIZlii. Sept. 26, 1886, Finlay, Cape of Good Hope, $100. Oct. 4, " Barnard, 100. Jan. 18, 1887, Thome, Cordoba, S. A., 100. Jan. 32, " Broolis, 100. Jan. 34, " Barnard, 100. Remuneration to judges, 75. $575. One gold medal to Edward D. T. Swift, for discovery of nebulas. ERRATA. Page 11, first line, for " Boss," read Prof. Lewis Boss, Albsiiiy. N. Y. Page 13, No. 12, for 11 8 4, read 11 18 4. Page 17, Nos. 33, 33 and 34 were discovered a short time previous by Barnard, of Vanderbilt University 01)servatory, Nashville, Tenn. LEWIS SWIFT. February 1, 1887. HISTORY AND WORK -OF- TLhc Marner ©bservator^, ROCHESTER. N. Y. 1883-1886. VOL. I. K0CHE8TER, N. Y. : DEMOCRAT AND CHHONICIjK BOOK AND JOB PRINT. TABLE OF CONTENTS. Page. Warner Observatory, Frontispiece. History, Descriptive Work, - 5 Tlie Dome, Section of 6 Comet Prizes, Awards of - 10 Warner Gold Medals, - 11 " " " Winners of, 11 Nebulae, Discoveries of, at Warner Observatory, - - 13-23 Comet Prize Essay, (Boss), 35 Sky Glow Essay Prize Winners, . . _ 31-70 The Warner observatory. HISTORY AND DESCRIPTION. THE Warner Observatory is distinctively a private institution built for the purpose of original discovery rather than the ordinary routine work of most other observatories. The desire of its founder was that the great telescope (then the third largest in the United States) be used In such work ; so, selecting as my principal field of labor, the discovery of new nebulae, which, since the death of the Hersohels and of D' Arrest, had been much neglected, and to which work the quest for faint comets had well trained my eye (an important factor), and also because of its congeniality to my taste (another influential consideration), on July 9, 1883, a thorough and systematic search was inaugurated for this class of objects, which were pop- ularly supposed to have been exhausted, a verdict which the fair measure of success, up to this writing, quite disproves. In this work occasional assist- ance has been received from my son Edward, now a lad of fifteen years, who has discovered twenty-one. These, in the accompanying published lists, are marked " Edward." When we reflect how much of bad weather has been had in the past three years, and that during a considerable portion of the time the moon puts a stop to the work, and that the seeing must be exquisite to reveal such exceed- ingly faint objects as have escaped all former observers, and also that about one-half of the clear moonless nights have been devoted to comet-seeking with the 4 1-2 in. comet-seeker, it will appear that the results are not at all discouraging. . DESCRIPTION OF THE OBSERVATORY. The frontispiece is a correct representation, copied from a photograph (taken from a point looking south). It is delightfully situated on the south side of East Avenue, one of the most beautiful and fashionable streets of this city. The building stands about one-third of a mile south of the University of Rochester, nearly one and one-half miles south of east of the Court House, and a few steps west of the princely residence of Mr. H. H. Warner, on what fifty years ago was a, dense forest. Its horizon is nearly unobstructed in every direction, in some points views forty miles distant being had. In nearly every outlook, woodland, field and meadow combine to produce most picturesque effect. The material used in its construction is white sandstone from Lockport — sixty miles west — and, unlike many varieties of this kind of stone, is free from red oxide of iron. The tower is circular in form, with a diameter of thirty-one feet, outside measurement. Its revolving dome is, of course, of the same diameter. This dome embodies some novel features, and in the matter of economy of construction, lightness, ease of revolution and simplicity of the device for rotating, leaves little to be desired. Hitherto nearly every principle of mechanical construction has been vio- lated in the building of observatory domes, and they have been made as 6 ■weighty as possible, under the delusive idea that if heavy they must needs be strong. Another prevalent error that has obtained is that powerful steam or gas motors are necessary to rotate them. To revolve the Warner dome, pulling or pushing— depending on the direction desired — on a perpendicular arm of tough oak, attached to the ring is all that is required, and this simple and inexpensive device is suflcient also for a dome forty feet in diameter, if properly made. I have seen this dome completely revolved by the hand of a boy of seventeen in i7 seconds, and, pulling with the middle finger of one hand, in 70 seconds. The only drawback to this ease of movement is its rotation, when the shutter is open, by the vrinds, which, however, is remedied by a simple device. In constructing a dome one essential is not to be overlooked, viz: the width of the ring or sole-plate, as it is this rather than its ribs that consti- tutes its sinews, as no matter how strongly it may be ribbed, the ring, after the wear of a few years, is liable to become elliptical, and therefore inopera^ tive beyond restoration. Our ring is composed of two thicknesses of 1 3-4 inch pine joined together with white lead paint (instead of glue and well bolted and spiked together. On the under side is bolted another thickness of the pine, though only as wide as the distance apart of the car-wheels, or about eight inches, which leaves on either side the upper portion projecting over the lower. Bach of the upper layers are 15 inches wide. To both inner and outer edges of this narrow under-strip steel wagon tire is bolted with coach screws, the former being two, and the latter two and a quarter inches wide, and 5-16 of an inch thick. These form the upper tracks, whose edges rest on the faces of the wheels. It must be borne in mind that the steel tracks largely prevent sagging of the ring between the wheels. The wall- plate is the exact counterpart of the ring, save that the narrow strip is at the top. The wheels, which are ten inches in diameter {and should have been fifteen), are flanged like car wheels, and are attached, one on each end of a short shaft. As I feared the machinist won Id fail to secure the exact relative proportions in size, the wheels were left loose on the shaft and may revolve if necessary. The pairs are not tied together, as it involves a useless expense not only, but also an increase of friction. Twelve pairs were at first used, but were soon reduced to eight. The dome is covered with galvanized iron, formed to fit the ribs, and riveted at the angles, as shown in fig. 1. The lower sheet is strongly nailed to the outer ^dge of the ring, and renders sagging between the wheels an impossibility. As in every direction the dome is an arch, and greatly stiff- ened by the angles, the ribs, except the two main ones, after the completion of the dome are of little use, save in the upper portions where they were found convenient as a foundation upon which to nail shoathing tn prevent the dripping of condensations. The condensations on the lower half, which is more nearly perpendicular, run down the iron and out between the angles. The ribs, Ave inches wide, are of 3-4 inch pine, twofold, with the lower ends merely nailed to the ring. The two main ribs are also of pine, thick and wide enough to project well above the outside of the dome, which prevents snow and ice from impeding the opening and closing of the shutter, which is worked by an endless chain. They are five feet apart, and the interval is covered by a single curved shutter which runs on gas pipe tracks off to one side, and may be opened to any width desired up to five feet. It is a great advantage to the observer to be able in time of hard winds to partially close the shutter. The estimated weight of the dome is 3 tons, while the weight of the Har- vard Observatory dome (same size) is 14 tons. THE PIER. The pier is round, 20 feet in diameter at the base, and tapering to 9 feet at the floor of the dome-room, where is placed, beneath the floor, a capstone 9 feet in diameter and weighing 8 tons. On this is built the rectangular pier on which the great telescope is mounted. THE TELESCOPE. The telescope was made by Alvan Clark & Sons, of Cambridgeport, Mass. Focal length, 23 feet; aperture of object glass, 16 inches; height of object glass from floor when pointing to zenith, 24 feet; interval between crown and flint lenses, 3.5 inches ; diameter of objective of flnder, 3 1-4 inches ; diam- eter of right ascension circle, 30 inches; of declination circle, 28 inches. The right ascension circle is graduated to 1 m. of time ; the declination circle to 10 sec. of arc. The tube is of steel, 14 inches in diameter at the eye end and enlarges to 18 in the middle and at the object end. When horizontal and in the meridian, the telescope is 51 feet above the surrounding lawn, 330 feet above lake Ontario, and 564 feet above the level of the sea. The optical center of the field of view is indicated by wires, visible with- out artificial illumination, crossing each other at right angles with another inclined at an angle of 45 deg., so that the difference both in right ascension and declination of a nebula from a neighboring star may, if desired, be quickly ascertained by counting the clicks of the telegraph sounder. THE MICROMETER. The filar position micrometer, of great excellence, was made by the Clarks. It has 4 eye-pieces with powers of from 195 to 1,250. The position circle is 6 inches in diameter. Gas instead of oil is used for the illuminant. The micrometer is not used in the nebula-work of this observatory. COMET SEEKER. This instrument (the telescope constantly used for nearly 30 years) is still employed in comet seeking from the flat graveled roof of the attached dwell- ing, which affords an admirable place for the work, though a frigid one in winter. DRIVING CLOCK. The driving clock is of the " Bond Spring Governor" variety, and works very well. It is started and stopped, the telescope clamped and undamped and moved to bisection, by means of cords, without descending from the observing chair, or even removing the eye from the telescope. THE OBSERVING CHAIR. The chair, which is strong and inexpensive, was designed with special reference to sweeping. Its seats fold upward at the will of the observer and thus render his position quite comfortable, while its curvature enables him to retain at every elevation the same relative distance from the eye-piece. A portion of it is shown in Plate 1. It runs on two parallel circular tracks of 7-16 square iron, and, therefore, no matter in what directional position it may be, cannot come in collision with either eye or object end of the tele- scope, which, when the room is absolutely dark, is a very assuring consider- ation. THE AUTOMATIC R. A. CIRCLE. Upon this exceedingly useful and time-saving device where right ascensions, already reduced to any desired epoch, are read off directly from the circle, I have, perhaps, from the want of a better, bestowed the above name. The privilege was exercised at the request of Mr. S. W. Burnham, its inventor, who endorses the appellation. I have spent much time and money in its improvement, and have finally succeeded in bringing it to a degree of per- fection unanticipated by either the original inventor or myself. Combining clearness with brevity the following is a description of its construction and manner of use. It, together with its severalacceasories, is shown in the illus- tration, Plate 2, copied from a photograph. A 15 inch circle of bronze gradu- ated to minutes of time and read by two verniers to 5s., and by estimation to 3s., is mounted on a short spindle attached (on a level with the eye) to the north side of the pier, close above the sidereal clock, and carries a grooved iron pulley about a foot in diameter. This, by a small pliant braided cord of fine brass wires, is connected with a similar pulley attached to the polar axis. A weighted rider presses on the cord which maintains the same degree of ten- sion under all temperatures. At first the verniers were propelled by a small clock regulated to sidereal time, but its rate falling to inspire the utmost confidence, thehair spring,escapement,and escapement wheel were removed, and, for the latter, a pin wheel escapement, with 39 pins was substituted. This is connected with a telegraph sounder in electric contact with the break circuit sidereal clock. The vernier clock is propelled as formerly by a spring the sidereal clock simply controlling the velocity of the verniers, which It does with an accuracy equal to its own rate. Above, and to the left ol the circle is seen a bottle of shot attached to a metallic cord wound around the shaft on which the verniers revolve. This takes up all lost motion caused by play between the cogs in the clock train. It must be understood that the circle moves at the same rate as the telescope and the verniers keep pace with the sidereal clock and of course with the apparent motion of the celestial sphere. With this arrangement the approximate R. A. of a new object is quickly obtained in the following manner. At the commencement of work the sounder and driving clock are started, the meridional eye piece wire accu- rately bisected on a neighboring meantime almanac star and the vernier set to its proper R. A. for a certain epoch, say for January, 1885.0. As my sweeping is generally confined to the meridian, or very near it, places are not vitiated by refraction. By a judicious selection of setting stars a fairly close approx- imation to the true R. A. of a nebula is read directly from the A. R. A. circle without making a figure for its reduction, save for declination in the usual manner. As the places obtained are purely differential the observer la relieved ol all anxiety about the time, the rate of the Howard clock only enters as a function of discordance. PLATE 1. General view, showing portions of dome, chair, entrance to little room, and telescope; and, in their entirety, the pier, clocl<, A. R. A. Circle, and pendant arm by which the dome is revolved. 9 After a nebula is found three or four minutes suffice to start the driving Clock, clamp, bisect, descend from the chair, read both the A. R. A. and dec. circles and write the record. Heretofore I have used apparent .nstead oi mean places for setting stars, but in future the latter will be used, which, owing to the unequal processional and nutational rates in different localities, will give better results. It is surprising that a contrivance of such utility has not come into general use. Of course absolute precision is not claimed, though the results com- pare favorably with those made with any equatorial, without the use of a micrometer and comparison star. THE SOUNDERS. As before stated the sounder controls the little clock which propels the verniers. The attachment consists simply of a short bar of hard wood, one end of which is bolted to the vibrating arm of the sounder, the other con- nects with the pin wheel escapement, which liberates a pin at each vibration of the armature, and which, during working hours, is kept consKantly going, being attracted to the magnet once in two seconds. By counting both the downward and upward clicks, seconds are indicated which are audible in all parts of the room. Counting these after stopping the driving clock mdicates by how many seconds a nebula follows or precedes a certain adjacent star. This sounder is also made to serve a useful purpose at the transit instru- ment. By taking in each hand an electrode connected by wires with the coil surrounding the sounder magnet, slight shocks from the secondary current are felt when the primary circuit is broken, and thus a transit may be taken as exactly as though within hearing of the clock beats. The wires in the dome room are concealed in the cracks of the floor. This sounder is therefore made to do a threefold duty. ALARM SOUNDER. .This is to awaken the observer at moonset or for inspection of the state of the sky. It is placed on a shelf attached to the bedstead of his sleeping room. Wires from the battery go to the break-circuit clock and to the sounder. Looking closely at the clock face in the cut, a false hand held by friction will be seen on the 24 hour arbor, and at the Dottom of the circle a metallic spring which the hand (previously set to the proper time for alarm) touches as it passes, and thereby makes connection with the battery. Suppose the moon to set at 2 A. M. and the setting is done at 9 p. m., the hand is simply turned five hours back from the spring, and, at its expiration the alarm sounder commences to beat and will continue for two or three minutes, insuring a thotpugh awakening of the sleeper. 10 SIDEREAX, CLOCK. This, the gift to me from a wealthy and generous citizen of this city, Don Alonzo Watson, Esq., was made toy the Howard Clock Co., of Boston, and gives perfect satisfaction. It is mounted in a niche iu the north side of the pier in the dome room, and is provided with a break circuit. THE SPECTROSCOPE. The only instrument of this kind now in use, is a small direct vision star spectroscope, though Alvan Clark & Sons have a contract to construct, at a cost of $1,000, a spectroscope to be used with either prisms or a grating, which is a present to the Director, from Mr. Hiram Sibley, of Rochester. ENTRANCE TO THE OBSERVING ROOM. This essential particular is in most observatories treated as a matter of indifference, though no door from any heated apartment ought ever to con- nect with an observing room. In this case, the entrance is by means of a staircase to the flat roof of the dwelling (where comet seeking is carried on, and where observations of shooting stars, northern lights, etc., are made), and from thence through an ample doorway into the observing-room. GEOGRAPHICAL LOCATION. Though circumstances have deferred the determination of the exact geo- graphical position of this observatory (a work which it is hoped will be done in the coming summer), it is assumed to bein Lat. + 43° 8' 35", Lon. 5h 10m 233 west from Greenwich, which in future is to be the prime meridian of the world. WARNER COMET PRIZES. When the Academy of Sciences of Vienna, Austria, had ceased longer to offer a gold prize medal for each detection of a new comet, Mr. H. H. Warner, the builder and founder of this Observatory, as an impetus to astronomical discovery in this country, offered in 1881 a prize of S200 in gold for every unexpected'comet discovered in the United States or in Canada. This offer has, with a few brief intervals, been continued down to the present time. Its last renewal dates from March 1, 1886, and is to ex- tend to March 1, 1887. The offered prize is SlOO, and is open to the entire world. Olber's comet of 1815, which is at any time liable to reappear, is in- cluded in the offer. Following is a complete list of the awards of the Waa-- ner astronomical prizes, with the names of the recipients, etc. : DATE. DISCOVEEEB. AM'T OF PKIZE. Oct. 10, 1880, - Swift, 8500. " Periodic" Special Prize. May 1,1881, Swift, 200. July 13, " - Schoeberle, 200. Sept. 17, " Barnard, 200. Nov. 16, " Swift, 200. Sept. 13, 1882, Barnard, 200. Feb. 23, 1883, Brooks, 250. Special PrizB- Sept. 1, " Brooks, 200. Comet of 1812- July 16, 1884, Barnard, 200. July 7, 1885, - Barnard, 200. Aug. 31, " - Brooks, 200. Dec. 2, " Barnard, 200. Dc<;. 26, " Brooks, 200. April 27, 188G, - Brooks, - 100. Mayl, " - Brooks, - 100. May 22. " Brooks, - - 100. — $3,250. PLATE 2. Showing A. R. A. Circle, verniers, sounder, vernier clock, star spectroscope, &c. Ij ESSA\S. Oomet Essay, Boss, - - .--... Bed Skyglow Essay, K. I. Kiessling, Hamburg, Germany, - " " J. E. Clark, York, Eng., " H. C. Maine, Rochester, N. T., U. S., - ' " " Rev. S. E. Bishop, Honolulu, S. I., Remuneration to Judges, - - Total, ' $300. 200. 1st prize. 150. 2d " 50. 3d " 50. 3d " 75. - $72.5. $3,975. There being a tie between the latter two essayists, Mr. Warner, instead of «lividing the prize, gave the full amount to eaoh. "WARNER GOLD MEDALS. Following are obverse and reverse illustrations of the Warner gold aaedals for soientiflo investigation and discovery. They have been specially awarded as follows, tor meritorious essays ou the recent sky glows : Prof. Cleveland Abbe, Washington, D. C. Prof. Winslow Upton, Providence, R. I. , Prot. H. A. Hazen, Washington, D. C. Prof. W. M. Davis, Cambridge, Mass. Frederick Cowle, Lauriston, River Forth, Tasmania, Australia. Rev. Robert Graham, L.L. D., Errol, Scotland. Dr. Charles Braun, Mariaschein, Bohemia. The judges were: Prof. Daniel Kirkwood, Bloomingtoa University, lud.; Prof. M. W. Hairington, University of Michigan, and Prof. Ormond Stone, University of Virginia. 'When, also, the building and maintenance of an observatory is considered, it must be generally conceded that Mr. Warner has been a liberal patron of science. The American Association for the Advancement of Science, appre- ciating this, in the year 1882 made him a member of that Societv. 1-2 DISCOVERY OF NEBULA. The subjoined catalogues of nebulEB embrace those discovered at the War- ner Observatory since July 9th, 1883. There have been, however, reserved foi' re-observation and the assignment of more accurate places, nearly one hundred others. In order that the non-professional astronomer may intel- ligently read the descriptions, a partial list ot abreviations, from Sir John Herschel's General Catalogue, and words for which they stand,are first given. an. another. B. brjg-ht. b. brighter, bet. between. c. considerably, diff. difficult. D. double. e. exceeding-ly. E. elongated. f . following. F. faint. G. C. General Catalogue. H. Sir Wm. Herechel. h. Sir John Herschel,hour8. 351, 582, 5251, etc. , refer to Nebulse. R. round. 8. south, seconds of time. B. p south preceding, s. f . south following. St. stars. sev, several. S. small. V. very. ♦ star. V a triangle. - degrees. ' minutes of arc. " seconds of arc. i. irregularly. inv. involved. 1. little. L. Large. m. much, minutes of time, magnitude. M. Messier, middle, u. north. neb. nebula, nebulous, neby. nebulosity, np. north preceding. nf. north following. nr. near, p. pretty, preceding, numbers In Sir John Herschel's General Catalogue of 13 CATALOGUE NO. 1 OP NEBULiE DISCOVERED AT THE WARNER OBSERVATORY. The places given are for 1885.0 and though only approximate, the nebulfe will, I think, be found very neai- the positions assigned. About a dozen were discovered by my son, then a lad of thirteen years. They are marlied "Edwai-d". All have north declination except those indicated by the minus sign. The eye-piece used is a periscopic positive, made especially for tlie worli by Guudla<;h of tliis city. It gives a power of 132, and the astonishingly large Held of 33'. Date of Disco very. 1884 Aug. 1884 Oct. 1884 Nov. 9 1884 Oct. 1883 Nov. 1885 1883 18SI 1885 1884 1885 18S4 1885 18EB 1864 1883 May 11 Aug. 24 " 24 " 24 April April 13 " 13 " 13 " 13 " 10 " 16 6 June 18 April 6 Mhv. 10 .June 14 April ^' 10 June 10 '• lOi July o 1885.0 01i4iii32« 2 2 3.5 2 27 32 2 4i a 3 1 31 3 1 32 6 20 36 9 23 SO 10 49 5 U 4 25 U 435 11 8 4 1138 40 1138 45 11 39 10 U 39 10 11 43 45 11 50 15 11 54 40 11 59 1 13 5 12 23 32 13 13 45 13 34 30 13 43 10 13 53 3 lis 57 13 57 39 18ffi May 9 " 11 1884 Juao 14 " 14 •' 14 1884 May 22 18S5 June 22 18S3 May 14 1885 June 9 • " 9 ' " 11 « •' 11 » " 11 ' " 11 1884 June 15 1883 July 11 ISSt May 21 1884 Auff. J 1884 Juno g 14 6 14 6 12 14 13 50 14 14 14 14 31 14 14 31 14 15 30 14 33 35 14 43 50 14 49 14 56 30 15 3 15 3 30 IS 4S5 15 10 15 1830 15 24 1625 16 89 5 16 44 8 10 45 9 la 45 10 10 48 30 d 1885.0 28-21' 7 25 Descjii ptions and Kemarks. 9 13 46 -2 13 6 40 27 38 11 20 10 23 15 68 745 18 13 30 22 21 30 22 23 21 1 20 8 42 20 3 43 20 27 20 12 37 13 42 43 56 1 40 20 235 05 5 40 19 39 35 51 26 54 40 12 20 -23 18 9 -29 ."iS 56 46 53 9 49 28 40 52 26 60 69 10 60 56 45 39 16 60 7!54 4 733 4 7 33 34 644 5 53 354 47 51 40 5G23 20 65 57 20 56 3 20 65 55 20 551145 54 57 13 8 15 60 8 13 20 25 27 CO 15 51 TO CO 28 TO 58 58 70 30 2S 71 23 e P ; V S ; E : B * nr- V P ; p S ; e E ; spindle ; cannot be G . C. 493, is not "am at," nearest* la 5* distant. Did not see 493, hut saw 523S H. descilptiou must apply to some other nebula. vF: cE. P: vE. S : B ; o P. Risrlit ang-lcd with 2 st. In field with Algol. eP; IE: vdiflT; F» close n. ^. ^ , , ,^ Nebulous » ; \- (liff .; B * exactly In center of L e P nebulosity; f , 1485 88» and is 10' n. Kesomblos 4634 in Cepheus, but IS fainter. pP;pS; E; IbM. p B : it ; no * nr. eeP: vS; It; diff.; s. of 2. vP;K; n. of2. , , . S ; V P ; f . <) Leonis 4«. Easily overlooked. vP:vS;E:B«lSsl; np. of 3. eP: K; pS; B*nf ; sf. of S. P; S; 1 E; 8 maif. * infield. vF; pS; R. :F; pS; ii P; vS; K; mb M. e P ; p Ij ; j) E ; V diff. ; D neb. nr. lanfrle. e !?■; p ij ; p Ej; V uiu.; ±i ncu. ui. . , ., ... l""*-";- p F • p b • K • n. of 3 St. which form with it a nffht angle trt S; f; vB; D * nr. e F ; V S ; p. nearest B t east 20». ceP; S; K; nearlybet.2st. p P ; K ; p L ; DM. noi-th 40''2844-5 point to it. e P ; p L; p. by 6b the middle « in a line n and s. oP; pS; IB; vP,f;p.diff. P ; V S ; to nu. * v close. t, . « ,j e F- S; 1 E; B«4'n: 2coarseD H,infleld. ... V P • 1) L : c E ; bet. 2 st. f ormius with 2 others a trap., the nC beinsr a fine D * of 2".5. Fii-st neb. discovered at this Observatory. I have not been able to see this object weU since its discovery, at which time I called it pB wlthp sharp outlines, but since the appearance of the red sunsets it has been ill defined and difhoult to see except as a hazy spot. This remark applies to all v F nebulae.* The D • is ppeP^'pS- B: eediff.; bet. 2 st. one a wide double. Edward. eecF; vS; K;eedJff.;formswlth2st.arightangletriangle. eF- n'S: K: F* nr. west. ,._ !• eP- IE- 2FBt.l)ointtoit; 2othersnr,; v dilT.; np.ofS. S '. e F '• St. ot 2 ; V diff.; a * midway bet. them. S;'eF:K; v.difl. V S- IE: vF: inbM. tonu. _ ., ..,.,, R • n S • k • P DM. north .52'>18163Ii. Found in presence of a half ' moon. 'First found 7 ycarsago with 4H inch Comet seeker and recorded as " can find no record of it.' P tp S ; K ; > ur.j saw another nr. as I supposed, but couid not reflncl it. vF;pS; IE; IBM;pB»nr. vp. E- pL; *nr.; 4058 in field. „ p ■' n A ■ K • v dill.; 3 St. in a line point to It: 4058 nr. eeF-pfeLlE:c diff.; p. a B , 7.; 4058 in field. vF: pX; 1B; in center of a L equilateral triangle ot uBst. F I V fe -"forms a right angle triangle with 2 st. e e ^ • V B ; F » at p. end ; vdlff. V F • S ; K ; coarse D * In field north. pF- pL: I E. 1st or 4. P;pL;B*nr. 2nd of 4. eP'E S. 3rd of 4. vF';pLjK. 4thot4. u No. Date of Discoveiy. a 1885.0 59 43 33 e P ; p S ; R ; 3 B St. nr. n ; 8. of 2. 05 tU li ^. 17 23 45 60 47 3 e F ; p S ; R ; 2 St. point to It, the nearer is D ; the other and the neb. are equally distant from U * ; n of 2. 68 " " 7 17 30 10 59 41 17 eP;vS;R. 67 1885 June IS 17 33 20 50 50 8 vF;S;R. [Edward. as 1835 Miiy 4 17 36 S'i 68 47 45 e P ; p S ; R ; f ormsji right angle triangle with 2 St., one m b. 69 1885 April 19 17 41 m 66 51 20 vP; pS;l{: BM. 70 " " 10 17 43 30 55 45 20 vP; pS; R; IbM. F: vS; R; BM. e P ; e S ; K ; e di£f.; stellar. May be a few o F et. 71 1835 Juno 6 17 42 4.-I 66 31 30 73 1885 April 19 17 43 40 55 49 2-3 73 1885 June 5 17 43 53 01 .53 F; S; R; planetary. 74 1S84 Sept. 18 17 44 30 00 57 30 eeeF:R; pS; ce diff.; s of 4 st. in form of a square. e P ; V S ; R : bi't. 2 St. which witli 3 others forms a cross like 75 " " 18 17 45 6125 33 cross in Cjgnua. Heb. placed ac Is j Cygui. 76 1S85 April 20 17 48 5 54 11 40 p S ; e F ; U ; 3 St. n. point to it, the n one the brighter. 77 1885 June 5 17 48 5 CO 6 10 e e e F ; p L ; 1 E ; bot. 3 St. e e dilT.; coarse D * s. 7S " " 18 17 48 4'l CI 33 40 e S ; p F ; V F * in or just in contact with it ; up. of 2. 79 ti H fj 17 48 55 01 83 20 F ; e S ; R ; planetary ; F * v nr. ; sf . ot 2. e P ; p S ; 1 E : diff . ; close s of middle » of 3 in a line, middle . the fainter ; np. of 2. 80 ISSt Sept. 10 17 49 30 69 31 17 81 " " 20 17 49 31 69 30 45 pF; pS; R; B*nr.; F, vnr.; sf. of 2. S ; V F ; forms with 3 St. a squaix'. 83 1884 June 17 17 52 30 72 I 58 83 1684 Oet. 17 .53 40 CO 49 ;53 F; p L; B M; 3 nearest of 3 St. in a curve point to it. V P ; R ; p L ; 3 St. in form of a triangle ur. Edward. F; pS; BM;R; bet. 2 8t. V F : V S ; R ; nearly bet. 2 st. 1st of 8. St 1854 Aug. 18 17 57 64 55 57 85 1885 June 8 IS 3 8 66 14 55 86 •' '• 14 IS 8 25 0124 87 " " 14 18 8 50 61 45 V S ; V F ; K ; l)et. a F and a more distant B ». 2ud of 8. 88 1883 Sept- 6 18 9 40 09 1 45 e F; p S ; R ; in vacancy ; 36t. in a curve south. V S ; R ; V F ; diff. by proximity to a B *. 3rd of 8. e P ; R ; p S ; nr. end of a curve of St. 4tli of 8. 89 1885 Juno 14 18 9 50 61 9 15 90 1SS3AUS. 4 IS 10 20 01 25 15 91 • ' 4 18 10 4.5 01 IS 5 ■ eP; pS; R; vdiff. 6th of 8. 93 " " 4 18 11 61 18 15 eS;R: vF; vF*nr. CthotS. vF; IE; pfe;P,*nr. 7th of 8. eeeF;pL;K:oe diff.; In vacanev. 8th of 8. pF; pS; IbM; R;nofa. Edward. 93 " " 4 18 11 5 01 IS 15 94 1835 Juno 14 18 13 40 61 16 45 95 " " 2 18 13 ."i.'J 68 19 20 90 " 2 18 13 M 6^ 10 5 p F ; p S ; R ; 1 b M ; s of 3. p B ; R ; m b M. Inx/ks like a comet. 97 1883 Sept. 11 18 26 50 73 6 15 98 1883 June 8 IS 33 23 67 3 10 pF; pB; R. 99 " " 8 18 33 30 07 45 ;» p F ; P S : 1{. 100 1883 July 11 18 36 69 33 17 e F ; p L ; R ; bet. S St., also bet. 2 coarse clusters np. of 8. 15 CATALOGUE NO. 'Z. No. 14 15 10 17 18 19 20 21 22 23 24 25 26 27 SO 31 32 33 34 35 36 37 33 89 40 41 42 43 44 45 46 47 48 49 SO 61 52 53 51 55 66 57 68 69 60 61 62 Date ot Discovery. 1885 Sept. 20 '^ 20 " " 20 20 1885 Oct. im Se^t. 17 1885 Oct. 1886 Sept. 1885 Aug. 1885 Sejit. 1885 Aup. 1884 Nov. 1885 Segt. 1885 June 1885 Aup. 1885 July 1885 Aug. 1883 Oct. 1885 Aug. 14 1885 July 8 1885 Aug. 1885 July 1885 Aug. 1885 Sept. 1883 Aug. 1885 Aug. 1885 July 1884 July 1885 July 1885 July 12 1885 Aug a 1885.0 01'0ni23« 52 2 22 3 30 8 43 8 45 8 65 9 6 20 60 42 50 61 40 1 1 30 1 36 10 1 41 10 1 50 60 1 50 60 1 66 50 1 57 10 1 .57 45 Z til 10 3 21 60 2 21 50 2 38 50 2 40 48 3 45 23 2 56 35 2 58 S5 3 3 43 4 6 12 6 15 6 24 11 8 1 35 8 8 8 11 8 11 30 13 45 60 15 32 5 15 32 45 16 8 15 16 15 33 16 29 45 16 30 16 41 30 16 47 16 56 40 16 69 16 69 17 1 10 17 .2.5 2 10 6 11 628 17 16 30 17 19 40 17 36 20 17 36 20 17 36 40 17 37 10 17 37 10 1,7 41 55 17 42 30 18 9 30 ,5 1885.0 18 9 28 IS 13 16 18 13 40 11118 13 40 12 32 37 44 21 30 -0 38 45 -0 41 37 43 10 80 16 46 46 27 6 46 24 19 4 29 39 36 38 40 46 2 41 44 42 67 43 86 46 40 66 27 84 30 -3 29 46 5 7 33 73 56 11 74 19 11 74 22 11 73 46 41 38 61 20 66 50 10 66 60 12 70 12 29 62 12 45 59 61 30 68 40 65 61 47 64 70 33 59 6 46 69 8 15 69 6 15 61 12 3 62 11 5 62 11 10 60 62 5 61 7 30 61 64 10 29 29 45 68 13 35 68 6 60 68 7 20 68 13 20 70 3 53 35 13 18 37 -19 55 1 —19 50 1 22 11 18 68 13 67 68 14 7 Descriptions and Bemakks. 81°50' 2"eF; vS; eE: B*s; vF* vnr. 32 17 40 eF; vS; K: bet.2st. 31 68 47 e F ; F. : V S ; one of 5 st. which point to it is p nr. 32 12 47 e e F ; ] E . in center oi; 3 v F st. forming an equilateral tri- angle, two of them double. 82 34 17 eF; S; IF. 47 36 80 e e F : p L ; R ; e difl. 1st of 3. 47 37 eeeF:SiR; middle one of S in a line. 2nd of 3. 47 86 45 p F ; p S ; R ; B M. Srd of 3. 81 4 15 e F ; V S : B ; forms right anifle triangle with 2st 31 19 45 eF; vS; R; v diff. 43 11 25 eeFilB:pS;iR;D* close f ; v difl. 39. 6 33 eF; eS; It; *nr. 13 50 pB;pL;vE: nearly bet. 2 p B st. If this Is Stephan's No. 1 of his Catalogue of 60 nebulae, A. N. 2390, then his descrip- tion is wroufJT in every particular. e F ; p S ; K ; bet. a D * ana a t, with a distant companion. v F ; p S ; IE; several st. nr. eeF; pS; B; n.of2. e e F ; B ; B ; s. of 2. e F ; p S ; i B ; D « close f ; v difC. eeF; vS; B; IbM; vdiff. eF;eS;R;lor2eF* close ; e difl. Powers 182, 200 ana265. eF;eS;R;B*nf;e difl. Powers 132, 200 and 265. pB; p S; B; p. apB»6i. V F ; p L ; E. V F ; p S ; D * nr. V F ; p S ; E ; * nrn. pF; pS; B. p F ; c E ; p S ; sev. v F st. nr. e F : V S ; B. Components of a nr D * point to it. vP; pL; B;lbM. Nebulous * ; e F ; p S : E ; p. G. 0. 1005 tii and is about 1'5 n. of it. Q. C. 1005 IS also a nebulouc * = H. V32, which Auwerfi describBS as being nr. and s. f . a B ,. This B « is the above nova. pB; eL; IE; H. VII; 2 near = G.C. 1424. pB; pL;lE;lbM;*nr. Edward. e e F ; p S ; R ; sev. B St. nearly surround it. e e F ; p S ; c E ; bet. an e F *, and an unequal D *. p F ; V S ; R. e e F ; p S ; B ; V diff.; 2 B st. nr. e S ; B ; stellar. eeF;vS:R;lbM. In field with G. C. 4114-15. V F ; V S ; R ; * nr n. pF;vS;E;«nr. Ltrlangle. V F ; p S ; IB; v coarse D * nr., forming with it an equilateral V F ; p S ; B ; F ♦ nr. pB; vS; R. e e F ; p L ; R ; bet. a B « and 3 st. in a line ; v diff. eF;pS;B. e F ; p S ; R ; * nr f ; 2 B st. nearly point to it. n. of 2. eeF:eS;B: s. of 2. e F ; E ; sev. v F st. nr.; v diff. p B : p S ; R ; bet. 2 st.; sp. ot 2. vP:eS; E; bet. 3 St.; nf. of8. V F ; V S ; 1 E. Close to 4278. sp. of 2. p F ; V E ; 3 St. in line point to it ; nf . of 2. V F ; V S ; R ; forms are of circle, with 2 St., neb. between, p F : V S ; R ; F * close ; stellar. eeF; e S; R; edifl. n.ot2. eeF; eS; B; ee difl. s. of 3. e F ; p S ; R ; nearly bet. a F anda B *. eeF; v S : B ; * nr. east; v difl. V F ; p S ; E. V F ; p S ; E ; 1 b M. vP; vS; B*f. 8b; bet. 2 st. A nebulous D * ; p F ; sf . of 2. A D * In center of a p F, p L circular atmosphere each* of the 8.5 mag. and about 30" distant. A wonderful object, not diff. Another D * in center of an e F, p L nebulosity ; np. of Z. Except the inequality oi the stars and the excessive faint- ness of the nebula, it won Id resemble the preceding. vF; eS;eE; foimsS. equilateral triangle with 2 F si. vF; pS; E; s. of 2. Double. V F ; p S ; E ; forma an e c.cBb double with the preceding. Very difBcult to separate with a power of 266. Well seen. No. Date of Discovery. o 1885.0 6 1885.0 67 1883 Sept. 1885 July 11 18 25 45 67 56 15 68 14 18 29 46 22 39 33 69 1883 Sept. U 18 30 50 67 54 15 70 1884 June 17 18 39 30 59 15 45 71 1883 Aug. 6 18 41 45 60 32 17 73 1885 Aug. 5 18 45 45 47 31 5 73 1885 Sept. 10 18 58 60 69 16 74 1884 Aug. 15 19 2 85 55 38 12 75 1884 April 30 19 4 30 63 44 60 76 1883 Aug. 30 19 4 30 63 45 20 77 1885 July 4 19 6 20 60 44 63 78 1885 Sept. 1885 July 10 19 14 20 60 )3 79 5 19 19 45 60 65 17 80 1885 Aug. 5 19 21 15 53 23 85 81 1885 Sept. 10 19 35 45 62 7 45 83 1884 Sept. 18 19 41 63 47 30 83 1884 Aug. 36 30 5 65 55 16 84 1885 June 9 go 18 30 66 28 10 85 1885 Sept. 14 20 33 35 65 42 12 86 4k it 14 20 36 28 65 21 43 87 '* " 11 21 10 11 50 83 1884 Oct. 10 21 30 45 12 16 54 89 >i 18 21 42 9 42 20 90 1884 Nov. 9 31 68 2 12 6 40 91 '* '* 9 21 68 2 12 7 40 93 " ** 18 22 35 10 — 5 034 93 ii it 15 23 47 — 9 51 32 94 1885 Oct. 31 32 52 37 13 41 22 95 1884 Oct. 14 22 55 20 6 742 96 a (I 14 K 55 30 640 43 97 it it 14 22 55 40! 6 740 98 1885 Oct. 31 23 3 S 11 25 49 99 1884 Oct. 10 23 6 30 30 29 43 100 1885 Oct. 31 23 21 40 11 45 4 Descriptioss and Eemarks. V F : V S ; R ; 2 St. range with it. pB;pS;R;mbM; bet. 2 st. Larger and b than 5918. vF; pL; IB; vFD*nr. e e e F ; in vacancy p L ; sev. B st. f . and p. it ; e diff. pB;pS;vE;F« close to f . end. vF; pS; R; IbM. vF; vS: R. p F ; v B ; 3 v F St. curiously placed in it on tiie line of major axis which also point to a D *. e F ; V B. s. of 2 eF; vS; cE; F*nr; D«in field, n. of 2. p F ; p L : c E ; sev. v F st. involved, e e e F ; p S ; 4 St. in semi-circle sf . ; e difl. T F ; p S ; V B in meridian. ]^';vS;R;*vnr;in field with 51 Draconis. eeF;pS;lB;a curve of st. w. like Northern Crown, e F ; V S ; F « nr.; v diff. Edward, p B ; R ; p S ; 2 B st. and it form an arc of a circle. eF;L;lbM;pB«nr. p B ; p L ; 1 B. Discovered many years ago with 4^ inch. eeer;pL;R;ee diff. p F; pS; R; IbM. Nebulous*; B«; ineeF nebulosity; v diff.; nearly pointed to by 3 St. in a line. V F ; p L ; 1 B ; bet. 2 St.; 5 st. w. in form of a pyramid. vF- S; R; IbM; s.of2. ee P; R; vdiff.; n. of 2. V F ; p S ; R. e F ; p L ; mistaken for Barnard's Comet 1884 II. [Pegasi. e e F ; L ; B ; F * nr nt.; V diff. Nearly in finder field with a eeeF; pL. K; s diff.; np. of 2. [Comet 188^1. eF;oB;p3*nrp. Found while searching for Encke'g eeF; p L; E; *nr. sf. of2. e F : 1 B ; S ; 9m , close nf. B ; p L ; R ; B M. Easy in presence of a half moon, e F ; p S ; R ; v diff. ; G. C. 4968 near ; H. is wrong and h. right as to brightness of 4966. 17 CATALOGUE NO. 3. No. Date of Discovery. « close f .; 16m ^ involved. 23 1885 Oct. 17 2 48 15 2 28 30 vF; pS; E; 1 b M. 23 1885 Nov. 10 2 51 55 — 8 13 40 eeF: S; K; *nr.8.; V difE.; sf. of 2. 24 44 44 10 2 51 23 — 8 940 e F ; p S ; B ; V ditf.; np. of 2. 25 44 44 10 3 12 18 — 8 3 lO e F ; e S ; E ; 4 B St. in form of arc of circle close south. 26 44 44 10 3 23 30 — 8 47 56 V L ; V E nearly in meridian ; e F. 27 1886 Feb. 24 348 68 17 5 vF; V S; R; B*near. 28 4V I* 24 3 53 36 70 43 55 e F ; p S ; R. 29 1885 Nov. 10 4 20 50 —10 22 29 V F ; p L ; E ; * nr. south. 30 1885 Dec. 29 4 28 50 — 8 49 55 S ; p F ; K. 31 15 4 39 22 — 8 41 24 e e e F ; e e ditf.; nf . of 896. 32 tt 4t i_ Date of ■"°- Uiscovery. a 1885.0 d 1885.0 1 1880 June 8 lOiOmlSi 18°26'58" 2 " " 8 16 20 18 26 58 3 " " 8 16 25 18 14 57 4 6 16 1 3 18 33 B 8 16 1 5 — 6 617 6 6 16 8 18 3 15 7 1886 May 22 16 9 15 61 32 4 8 1886 July 3!l6 10 52 1 9 22 9 6,16 17 58 16 45 SO 1886 June 28 16 17 6 58 16 20 ai " 28 10 17 24 57 64 5 12 1886 July 9 16 18 5 65 10 30 ia 6 16 18 32 56 15 3 14 1886 June 28 16 23 16 55 37 18 35 1886 July 9 16 25 5 69 44 13 i6 6 16 30 59 2 30 37 1886 June 28116 33 35 57 44 5 ae 1886 July 9 16 34 50 62 11 25 a9 3 16 45 1 4 49 29 so 1886 June 28 16 45 55 62 21 10 a " 28 16 46 55 63 24 40 22 " 28 16 47 25 55 44 32 23 " 28 16 50 50 80 43 8 24 1886 June 9 17 1 55 60 32 21 25 1884 Aug. li 17 25 20 58 35 10 26 i;i7 25 30 58 36 65 27 1886 May 30 17 33 45 74 26 5 28 1886 June 9 17 43 55 67 38 4 29 9 17 44 30 67 38 4 SO 1886 May 30 17 45 45 51 10 10 SI 1884 May 27 17 51 5 65 34 12 32 1886 May 30 17 53 60 49 30 33 " " 28 17 53 30 62 39 20 34 " '■ 28 17 63 50 62 40 20 35 " " 28 17 54 20 62 38 20 as 1884 July 24 17 54 44 50 45 15 37 1886 May 30 17 56 35 73 25 31 38 1886 June 6 17 56 45 19 42 15 39 " 28 17 56 45 64 18 42 40 1886 May 27 17 59 45 66 35 25 41 1884 July 23 18 22 66 33 26 43 1886 July 30 18 33 66 51 15 43 1884 Oct. 25 18 33 30 67 55 44 1884 Aug. 16 18 36 55 55 30 13 43 1886 May 27 18 45 45 66 35 55 46 1883 Aug. 20 19 15 40 63 44 35 47 1886 June 5 20 35 55 65 40 25 48 1886 July 12 21 36 46 12 3 31 49 1884 Nov. 9 23 11 45 28 23 40 SO 9 23 12 30 28 23 10 Desckiptio.s anu Remarks. eeeF; S; E; eedlff. Ist of 4. eeeP; S; R; eedilf. 3nd of 4. eeo F; pS; K; ee dilE. 3rd of 4. eeeF; S; K; eediflf 4th of 4. 4 B st. with the neb. form a cross-like cross in Cygnus: neb. placed as is Deneb Cygni. V F J S ; R. eoeF;pS;eee difl.; R. e F ; p S ; R ; in line with 2 st. [e e diff. e e F ; V S ; a B and a F * nr. np. point to it, an e e F , close p ; e F ; V S ; R. 1st of 8. » u=c p , p F ; p S ; R ; B M. 2nd of 3. p P ; p L ; R : B * nr p. 3rd of 3. V F ; V S : E ; 2 St. nr. eeeF; S; B; nearly bet. 5 p Bst. in a curve n. and 3 Fst. in a curve s.; e diff. eeF; pS; E; vdiff. e e F ; v S ; R ; In vacancy. Many p B st. s.; e diff. p F ; p L ; E ; 2 St. nr. p. V F: v S ; E; forms right angle triangle with 3 st. 1. eeF; p S; « near f. eeeF; p S ; R ; bet. a distant B » fanda distant F , p.; e o ditt. eeF;eS; eF* close; e diff.; sp. ol 3. / y F; vS ; R; bet.2st.; nf. of 3. eF; S; R. eF;vScR;aB* and a D « nr. p. eF; S; cE; F *.jir. vF; S: R; sp. of 3. v F ; S ; 1 B ; * nr. nf. of 2. e e e F ; p S ; B ; bet. 2 St. 4 F st. nr. p form arc of circle. eeF; S; R;pof2: ee diff. eeF; S; R;f of 3: vdlfE. p B ; S ; e E ; spindle. In field with Gamma Draconis. e e F ; V S ; R ; bet. 2 pairs of coarse D st. e e F ; p S ; 1 E ; e difl.; in vacancy. Only 1 v F « nr. e F ; p S ; V E. 1st of 3. ee F; vS: R; pB*nr.p, V difl. 2nd ol 3. eF; pL: 2Bst. nr.f. 3rd of 3. V F; V S ; H ; 2 B st. nr.; in finder field with Gamma Draconis. eF; vS; IE; bet. 2eF6t. eeF; vS; E. eeF; pS; R; in center of a semi-circle of 4 st. e F ; S ; 1 E ; H. 37 I V in field, e e e F ; p S ; E ; forms triangle with 2 st. eeeF;pS;lE;lbM;ee difl. ; 2 or 3 others in field, e F ; e S ; bet. a v close * and a v F D *. V F ; p L ; R ; p B « nr. s. eeeF; pS; ee diff.; several B st. nr. u. eeeF;pL;R;ee difl. p B; p S ; B ; mb M ; p B * nr. eeF;S; R; pB* with distant companion close p ; v diff. vF; iR; np. of 2. V P ; p S ; R ; D , nr. sf . of 2. 20 The following nebulEe were discovered after the partial Catalogue No 4 was put in type, and are, therefore, arranged in the order of discovery Instead of R. A. No. Date of Discovery. al885.0 h m ■ 1 1886 July 22 14 69 30 2 " " 22 17 26 4 3 " " 22 17 26 24 4 " " 23 17 58 25 6 " " 22 17 45 6 " " 22 17 45 7 " " 31 18 30 55 8 " " 31 18 32 5 9 " Aug-. 3 33 125 10 " " 3 16 38 53 li 5 16 54 35 12 5 16 50 55 13 8 17 1 35 14 1884 Auj>. 15 17 20 30 15 " July 24 18 8 16 1886 Aug. 5 19 25 17 1884 June 18 18 35 40 18 " Nov. 9 S3 15 15 19 1886 Aug. 6 23 55 15 20 " " 5 33 56 10 21 1883 Aug. 31 23 6 30 22 1886 Aug. 8 33 4 35 23 8 23 14 45 24 8 23 33 45 25 9 23 46 38 26 9 38 30 27 9 30 26 28 9 36 29 " " 18 17 17 10 30 " " 31 21 20 40 81 " Sept. 1 17 23 45 32 " '• 1 17 23 40 33 " ■' 1 17 36 55 34 1 17 47 58 35 1 32 9 55 36 1122 16 30 37 1 32 26 30 38 133 18 40 39 133 39 40 1 38 40 41 1 1 46 50 43 1 2 30 5 43 1 3 13 50 44 2 22 38 45 2 32 49 5 46 2 22 49 5 47 2 23 40 45 48 2 33 47 45 49 " " 3 1 9 30 60 3 3 140 51 3 10 46 10 53 3 19 45 35 53 6 19 59 55 54 " " 6 33 10 55 55 6 23 6 60 65 6 3 2 20 57 6 2 30 47 58, 7133 39 20 59 1885 Oct. 30 3 37 30 39°57'20" 57 37 11 57 38 11 61 22 5 57 30 55 67 21 10 67 3 53 59 48 15 27 34 66 15 25 63 35 16 63 54 30 61 13 30 63 16 15 49 53 30 54 8 30 71 31 23 25 16 18 12 29 6 13 20 36 14 30 10 34 24 26 41 13 26 21 10 50 10 -10 20 7 -10 45 20 -10 38 48 60 44 5 13 4112 58 55 33 58 55 18 58 56 33 62 15 45 21 56 53 — 4 41 18 11 7 24 13 20 36 15 26 15 —11 33 25 11 38 54 11 8 56 — 2 23 24 8 6 12 38 50 12 30 30 20 29 2 7 28 45 — 3 13 33 16 39 30 59 37 59 37 65 55 10 16 45 13 6 22 3 39 44 20 35 53 — 8 19 5 31 .59 31 Descriptions and Remarks. eeeF;ps; le;ee diff . eF; S; K; spof 3; B * nrs. e P ; S ; B ; nf of 2. This and the above point to the 3*8 magnitude, e P ; S ; e E. Course D « sp points to it. e e P ; S ;• K. 1st of 2. e P ; p S ; R. Sst In a line nr and 3 others in a line point to it 2nd of 2. p B : p S ; V B. e e P ; S , B ; bet a F and a p B « ; nearer the former ; ediff. vP; S: R. e P ; V S ; R ; forms a L equilatera. a with 2 p B st. eeeP;S;lE;lbM. Nearly in center of a L vacancy; e e diff. e F; p S ; R ; 4 or 5 st near sf in form of a curve. e F; p S ; c B ; sev. v P st close p. e e e P ; p L ; i R ; sev. e P st involved ; B st nr sf . e e P ; p S ; E ; in vacancy bet 6 st like sickle in Leo, and 4 like Alpha, Beta, Gamma, Delta TJrsEe Majoris. eP; pS; H; P*nrs. e e P ; p S ; IE; bet a near F «, and a distant B one. e P ; p S ; R. pF;pS;R;P*v nr. np. Nearly bet the 2 p of 3 st in line ; np of 2. Neither place nor description agree with 5044. p P ; D S ; R ; 2 P st nr in line with it. Not dift ; sf of 3. V F ; S ; R ; bet 2 St. e F ; V S ; R. pF; pS; cE; 3stina line near np. eeP; pS; R; p B , nr f ; ediff; 6218 nr nf. e F ; S ; R ; in center of equilateral a of 3 st ; D , nr np. p P; p S; R; * nr nf. 3 F ; V S ; R ; V diff ; only 1 * near. V F ; p S ; R. V F ; p S ; e B ; spindle.nearly bet 3 p B distant st ; nearer the Pt e e e P ; close st of middle of 3 F st in a curve, middle f the brighter, e e o diff. Nebula nearly in same parallel as the s * of 4 in a row p. e F ; e S ; R ; e diff.; in center of equilateral a ; np of 3. eeP; eS; R; ee diff.; sf of 2. e P ; V S ; R; nearly between 2 st. p P ; p S ; B ; between 2 st and 3 st in form of a semi-circle. p F ; S ; R ; mb M; 4 st in form of a square, near p V P ; p L ; R ; 4 st nr sf point to it. e P ; S ; R ; in center of 4 F st In form of a rhombus, e P ; S ; E ; in vacancy. V P ; V S ; E ; 2 st point to it. pF; S; R. e P ; S ; R ; B * nr f . V P ; S ; R ; B M. forms trapezium with 3 St. vP; S; R; 4stf ina row. V P ; S ; R ; lb M. eeeP;S;R;eee diff.; n of 2. e e P ; p S ; E ; e diff.; 8 or 10 st in an irregular line p ; s of 3. e P ; V S ; E ; forms equilateral a with 3 St., one the brighter. e e e F ; p S ; R ; 5025-6-7 and 8 in field. p B ; V S ; 1 E. e F ; V S ; R ; right angled with 3 st. e P ; S ; R ; f of 2. eP;pS;H;pB* close s.; p of 2. p B ; p S ; R ; B M. V F : V S ; R ; 3 st sf form a little right angle i . e e P ; S ; H ; e diff.; 5 or 6 st nf in a line. pP; pS; R. p F ; p S : E ; * near s. e F ; p S ; E ; * nr s, which with one f and p forms a doible a. p e F ; V E ; p B ♦ nr sp. 21 THE GREAT NEBULA IN MONOCEROS. This interesting nebula is a nova, discovered some fifteen years ago, while comet seeliing with the i}4 inch telescope. After satisfying myself that it was not a comet, it seemed probable that it might be simply a glow from the well-known cluster H 2, VII, to which it closely adjoins, liut, finding the glow confined to one side ouly, I became convinced that it was a nebula, and being so bright and large, doubtless previously discovered. Obtaining Herschel's G. C, I found, by its absence from the list, that it was new. Two or three years ago, Mr. Barnard picked it up, mistaking it at first, as I had done, for a comet. On one very fine night, before the appearance of the red sunset phenomena, the 16 inch refractor showed it as elliptical with a center of condensation at each foci, as roughly represented in flg. 2, which was Fig. 2. sketched for and published in the Sidereal Messenger. And though on no subsequent occasion have I been able to see it as illustrated, yet I have since observed another near, itself very large, with two or three contiguous out- liers. The Monoceros nova is one of the largest nebula visible from this latitude. Its approximate position for 1886.013 6 h. 24 m. 45 s.. Dee. -|- 5° 7' 40". It is somewhat brighter than the Merope nebula in the Pleiades. THE SWAN OR HORSESHOE NEBULA Proves to be a most wonderful object for study. It, however, bears scarcely the slightest resemblance to the pictorial representations as published by Lord Rosse, Trouvelot, Lassell or the Herschels. The accompanying wood Fij;. 3 r2 cut, fig. 3, is, however, poorly illustrative of it, though it will serve to give the reader something of an idea of its extent and unique form. This object is in the Milky Way, a region which, though rich in star- clusters, yields very few nebulas. It is No. 4403 of General Catalogue and 17 of Messier's. Its approximate R. A. is 18 h. 14 m., Dec. — 1G° 13'. The illustration, originally prepared for the Sidereal Messenger, for March, 1885, was sketched from memory and, of course, not to scale. The singular ap pend- age at the following end has, as far as I know, never before been seen. It was first noticed on July 4, 1883. It was again seen the next evening, and, on July 6, was corroboratively observed by Messrs. Warner and Rebasz. Sub- sequently, on the occasions of their visits to this Observatory, after their attention had been directed to it, it was thus seen by both Dr. Copeland and Mr. Trouvelot. There is much of detail in it, and needs to be drawn to scale, by an expert, for adequate representation. I have not been able to trace the appendage to the pretty large, exceedingly faint nebula just pre- ceding its termination, but have no doubt that, with a larger telescope, a coalescence would be detected. This latter isolated nebula is a new one. SECONDARY TAIL TO PONS-BROOKS' COMET. This coniet presented many curious freaks, but its most interesting feature was a secondary tail of peculiar shape, seen only on the evening of December 29, first, by the writer, and after, by Mr. Streeter, an astronomical friend, who was visiting the Observatory. Fig. 4. The cut, fig. 4, is an exact inverted delineation of its appearance at that time. The primary tail could be traced about 8°, and the secondary about 3°. The latter was an exceedingly difficult object to see. Both were perfectly straight. Secondary tails are not always shortest, as, c. g., on the evening of June 26, Comet II, 1881, exhibited, to the naked eye, a secondary tail extending to Pi Draconis, or some 55° or 60° long, which was seen by several visitors to my former Observatory. On the next evening, though the conditions for seeing were equally good, it had diminished more than one-half. This is the longest secondary tail extension I have ever seen recorded. LEWIS SWIFT, Director. Waknee Obsebvatory, Bochester, N. Y., U. S. A., January, 1887. The Warner Prize Essays. In the Order in which tney were Awarded by the Judges. U.i THE WARNER COMET PRIZE ESSAY. Comets: Their Composition, Purpose and Effect Upon tlie Earth. By Professor Lewis Boss, Director of Dudley Observatory, Albany, N. Y. In January, 1881, Mr. H. H. Warner, of Rochester, N. Y., Founder of the Warner Observatory, announced a prize of $300 in gold to any American or Canadian who, during the year, should discover a telescopic unexpected comet. When Comet "B," or the great comet, was discovered, effort was made to ascertain who first saw it, and had a conclusion heen possible among the very many of claimants, a special prize would have been given. As none could be reached, Mr. Warner determined to give a special prize of $200 for the best essay on " Comets, their Composition, Purpose and Effect on the Earth." One hundred and twenty-five essays were sent in to Director Swift, of the Warner Observatory, and after a careful review, the Judges — Professor Elias Colbert, of Chicago, 111.; Professor H. A. Newton, of Yale College, New Haven, Conn.; and Professor H. M. Parkhurst, of New York City,— unani- mously awarded the prize to the essay signed " Hipparchus III," by Profes- sor Lewis Boss, Director of the Dudley Observatory, of Albany, N. Y. Following is the full text : Though modern science has taught us much concerning the physical nature of comets, no one has yet been able to construct a theory which is either complete or free from objection. With these facts in view, and so far as possible within our brief limits, and without the use of technical lan- guage, we will endeavor to outline some of the more important results of observation and reflection upon this subject. We shall be obliged to draw freely from the results elaborated during the last fifty years by Bessel, Winnecke, Bond, Newton, Zoellner, Bredichin and many others, without reference to individual authorities, or digressions upon rival theories and claims. METEORS— OFFSPRING OF COMETS. § 1. About twenty years ago it was proved that certain annually recur- ring displays of meteors are due to swarms of small bodies, which revolve about the sun in elliptical paths, so situated in space as to encounter the earth at nearly the same time in each succeeding year. These paths or orbits were found to be identical in some oases with those of certain well known comets. The conclusion seemed irresistible and is now accepted, that shooting stars, or meteoroids, are simply the offspring of disintegrated comets. Most likely, aerolites [large meteors] which sometimes reach the surface of the earth, are of the same origin. These bodies usually enter our atmos- phere with velocities [relative to the earth] ranging from twenty to forty- five miles per second. In consequence of the inconceivable heat which (25) )i<6 would he generated Ijy such contact— manifes*ed by the fiery train thev leave behind — the smaller meteors, however dense, vould be at once con- verted into impalpable vapor. Only the larger ones could survive tiic tremendous encounter, and reach the earth. Still other composed of moie fusible substance, though very large, may be unable to either overcome the mechanical resistance of the air, or the transcendent heat produced. Furthermore, that fiery ordeal must strip aerolites of all volatile matter and leave only refractory substances behind Hence, analysis oi meteoric stones might, give us an idea of the real composition of comets vchich would be totally misleading; just as the rums of a house, destroyed by fire, would be no index of the chemical composition i^f all the material it contained before the disaster. TESTIMONY OF THE SPECTROSCOPE AND POLARISCOPE. § 2. The Spectroscope [light analyser] rather reluctantly yields some testimony as to the chemical and physical nature of comets. It seems to show that the nucleus Is a solid or liquid incandescent [at a glowing tempera- ture] mass. It proves quite conclusively that the matter surrounding the nucleus contains hydrogen and carbon in one ox' their numerous compounds. The flame of the Bunsen burner which contains one of the compounds, shows a spectrum [light analysis] which is very similar to, if not identical with, that observed in comets. Some observers have reported that these elements give evidence of their presence in the tails of comets at considerable dis- tances from the head. If so, we must suppose the attenuated matter of the tail to be self-luminous. This may be attributed to some form of electrical action ; since, considering the low temperature of space, it cannot be due to incandescence produced by ordinary heat. Recent observations with the spectroscope seem to prove that a part of the light from comets is really reflected sunlight, since it faintly exhibits a spectrum like that of other bodies, which shine by reflected light alone. The Polariscope [instrument for detecting reflected light] also gives evi- dence which leads to the same conclusion. The use of this instrument in examining faint sources of light is attended with great difficulties ; and in the present connection, the records of different observers are not strictly harmonious. RECORD OF THE TELESCOPE. § 3. Comets are seen in their simplest form as faint patches of nebulous light. They are usually circular or oval in outline, without remarliable difference of brightness from center to ciroumf erence. At a later stage of development the comet shows a diffuse brightness in its central parts, known as central condensation. . When a large comet approaches the sun, the structure becomes far more complex. The center condensation gathers intensity. Finally, a point or disc of light appears near its center, which shines with a light approximating that of the planets. This is called the nucleus. ISrUCLEUS HAS NO DEFINITE MAGNITUDE. Observers with powerful telescopes usually find that what we commonly call the nucleus has no definite magnitude. It continually measures less with increase of optical power. The inference is that the real nucleus, if it consists of a single solid body, must be very small, and much obscured by the vapors which surround it. Generally the nucleus appears to shrink in size as it approaches the sun. The most plausible explanation seems to be, that with lessened distance from the sun, the real nucleus gets hotter and brighter, and that, at the same time, the vapors near it become more trans- parent. Other explanations have been offered which we have no space to consider. - I THE EXVBLOPES. We commonly find that the coma [nebulous matter about the nucleufi] appears much brighter ou the sunward side. la mauy cases, streamsof matter appear to issue from the nucleus on that side. These assume a varietj- ol forms, and are almost always curved backward, from the direction of tlj<; Sim, at their extremities. Above the streams, or jets, are sometimes seen one or more arcs of light, ooucentric with the nucleus from which they appear to recede, — just as waves recede in widening circles from a stone dropped into still water. These envelopes, as they are called, are supposed to be hollow spherical segments of matter, more dense than the surrounding parts of the coma. One highly important characteristic of the matter which surrounds the nucleus is well established. The rays of light from distant stars seen through it are not sensibly bent, or refracted. This shows that gases of an appreci- able amount do not exist in comets. THE PHENOMENA OF THE TAIL. The strange appearance of the tail and the gigantic dimensions it some- times attains, are well calculated to arrest the attention of mankind. It is not wonderful that the ancients should have regarded it with trembling apprehension, nor is it surprising that, even yet, it excites an absorbing curi- osity among the educated, and the superstitious terrors of the ignorant. The matter of which it Is composed must be expanded to an almost incon- ceivable degree ; for even when it is millions of miles in diameter, the light of the faintest star is seen through it with scarcely diminished brightness. THE BLACK STREAK IN THE TAIL. Near the head, it often appeals to consist of two streams of matter issuing from either side of the coma with a dark channel of separation between. The tail at thispoint generally appears to have the same diameter, from what- ever direction in space it is viewed. Wo must, therefore, conclude that its interior is nearly or quite free from matter, and like a hollow cylinder or portion of a cone, as far as the dark channel extends. Beyond that point we may suppose that the interior fills up by gradual diffusion from the cir- cumference. In some cases, and especially with small comets, the dark channel is wholly wanting, or but faintly indicated. CURVED DIRECTION OF THE TAIL. In order to give an idea of the situation of the tail in space, let us imagine a line from the sun con tinually prolonged through the moving head of a comet into space beyond. We shall always iind the tail extending nearly opposite the sun, in the general direction of this prolongation, but curved more er less backward from it, in the direction from which the comet is moving. Sometimes we find more than one tail— each distinguished by the degree of its backward inclination. They have, indeed, been classifled on this ground and found conformable to three general types. ORIGIN OF COMETS. § 4. The facts thus far presented prove nothing as to the origin of comets. That question demands for its solution mathematical reasoning based on the calculated paths of all comets which have been observed. That discussion is beset with great difficulties, and as yet points to no absolutely certain conclusion. The balance of testimony seems to favor the supposition that comets originate outside the solar system. The planets move in nearly circular orbits about the sun ; and no one has been able to show why comets, if they have the same origm, should move in elongated orbits, entirely differing from those of planets. 28 Let us suppose, liowevei-, that all comets must have takeu their origin in some primeval nebula from which a solar system has been evolved. It has been shown that the velocitj- of a comet may be so much Increased by the disturbing action of a large planet, that it may escape from the control of the sun, and be projected into the illimitable regions of space. Thus freed, it will go on in a nearly straight line forever ; unless, perchance, some jjow- erful source of attraction, like another sun, lying near its path, arrests its flight. The possibility of such an occurrence is by no means imaginary. At least one comet [Lexell's, 1770,] is supposed with good reason to have under- gone that fate. There is every reason to believe that the same thing may have happened in other cases. STELLAR COMETS. All argument drawn from observation and reflection prove that the stars which surround us on all sides are remarliably lilie our own sun. Some of them are even larger and more powerful than he. Reasoning from analogj-, we must suppose than these suns are also attended by comets. Hence, we are led to the conclusion that uncounted myriads of comets projected forth _ from millions of suns, during countless ages past, are now flying through space in every direction — restless messengers from star to star. By mere chance some of these bodies must come under the suns far reaching power and be drawn into our planetary system. PHYSICAL HISTORY OP COMETS. § 5. The mass [quanity of matter] of comets is conceded to be very small in comparison with that of the earth. How small it is, we cannot say. No comet has been found large enough to exert a sensible attraction upon any celestial body found in Its vicinity. This fact confirms the conclusion derived from telescopic examination, that the real, solid nucleus, if It exists, must be extremely small. It is certain that no body entirely gaseous could exist in space. The con- ditions for the stability of liquid bodies in their practical application to the explanation of cometary phenomena, are extremely complicated; since they are closely associated with the unknown elements — mass of the comet, solar radiation, and absolute temperature of space. It would also be extremely difficult to show how a swarm of small bodies could be preserved in a state of equilibrium, or resist the tremendous tidal action to which it would be subjected in the vicinity of the sun. In fact, we must Tiew the conversion of a comet through some unusual catastrophe, into such a swarm, as the sure precursor of approaching dissolution. On the whole, it is prob- able that there is a solid or partly liquid body near the center of uhe comet. This body is more likely to consist of an aggregation of loosely cohering pieces or particles, than of a single, flrmly-united muss. Owing to the smallness of their attractive force, comets cannot retain a sensible atmosphere. This conclusion is confirmed by telescopic observation, as we have seen. If, now, we suppose the nucleus to be approaching the sun, it will event- ually reach a point where the liquid or other volatile matter on the "sunny" side commences to evaporate and be diffused about the comet, ^yithout following the consequences of this evaporation into details, one can imagine for himself how the appearance of central condensation, of the streaming jets, and of the nucleus heavily obscured by vapors, might be produced. To acoonnt for the backward curvature of the jets and the peculiar form and direction of the tail, we must look for some additional force. In all probability this force resides in the sun, and ij directly opposite in Its effects to the power of gravitation. But since the bod/ of the comet obeys th j law of gravitation with sufficient fidelity, we must find a repulsion which sensi- bly acts only on the molecules of gas or viqior. 29 The only force suggested by experience as oonipetent to these require- ments is that of electrical repulsion. Anyone can prove for himself that two bodies similarly electrified mutually repel each other. We know that the earth through effects of constant evaporation and other causes, is to some extent an electrified body. For the same reasons, we should expect comets to be electrified in a much higher degree. The sun itself certainly exerts an Influence upon terrestrial magnetism. Violent commotions on its surface have occurred at the same time with unusual disturbances of the magnetic needle. Electrical repulsion acts in proportion to surfaces and not to vol- umes. On particles of matter in a state o£ infinitesimal subdivision it might act most powerfully, while not affecting a large bOdy to an appreciable degree. THEORY OP rORMATION OF TAILS. If, then, we suppose the sun and comets to be sufficiently and similarly electrified, we have the force necessary to produce the backward curvature of the jets, and to drive off the smallest and probably outermost molecules of the coma to form the tail. Since, according to our hypothesis very little matter can be given off from the shaded side of the nucleus, we readily per- ceive why the tail should be hollow in appearance. The orbit of the moving nucleus being curved, it is evident that the par- ticles driven off at any time with less than infinite velocity, would continu- ally fall more and more behind the prolongation of a line through the sun and comet — just as has been observed. If the matter contains molecules, varying considerably in size, the larger ones would be driven off with less velocity. These would curve backward more than would the lighter mole- cniles driven off at the same time ; and so we have the multiple tails which have teen seen, as well as the classification already described. Elaborate exam- inations of their average observed direction and form suggest that each class may be composed of chemical elements peculiar to itself. We may even venture to suppose that the tail of greatest velocity and least inclination is composed of hydrogen. The second type may contain carbon, with or with- out other elements ; and among those of the third, chlorine would most likely be found. It is a common error to suppose that this hypothesis, as to the f orma/- tion of the tail, requires a repulsive force of inconceivable power. The straiglitest tails which have been observed are accounted for by supposing a repulsive force not much greater than twelve times the sun's attractive power. The tail most frequently seen [scimeter-like in form] may be pro- duced by a force about one-ninth of that amount, which is but little more than sufficient to overcome the attraction of gravitation. It will lie seen that it is equally erroneous to suppose any great amount of material wasted in the formation of the tail, when one reflects upon the transcendent lightness of its structui-e. HOW COMETS AFFECT THE EARTH. § G. The influence of comets upon the earth is in all probabiUty quite insignificant. They may, like the sun, affect the earth's magnetic condition, and thus to some extent, possibly, its meteorology. No such effect has ever been perceived. In spite of some chanr. Hellmann ; See Kiessling' s^* Ikeamnerungserschevnwngen ira JofirclSSS." P- «• + idem, pp. 43-53. (39) 40 Similar appearances became rapidly common over both Temperate Zones, and have re-appeared at intervals ever since. The writer's observations at York, (occasionally at Street, Somerset,) represent 16 "periods." The main points are summarized in the table on opposite page. Selecting for comparison the maximum of the 67 sunset glows, the wax- ing and waning is very notable, minima coming at the 4th, 8th, 13th and 15th periods. Curiously, an increase occurs on each anniversary of the Krakatoa eruption. The morning and evening effects were obviously alike ; yet meteorologi- cal changes often modified their development. Regarding, then, sunrise as simply sunset reversed, the following sunmarizes the writer's personal observations : A "glory" surrounded the sun. At first it was, for 10°, "yellow," or " tawny" and the next 15° to 30° " rose or salmon-colored, gradually chang- ing to ordinary tints ; the clouds grey -green in contrast." After 1883 the inner part assumed an exquisite silvery, sheeny look, or was entirely absent, the rose approaching nearer the sun, if that were under a cloud. On approaching the horizon the glow grew " tawny" or " muddy." About 10 minutes after sunset, the opposite sky became tinged with dusky rose, — the Counterglow culminating at 25 minutes to 30 minutes, in a Counterbow, almost semi-circular, resting upon the Counterglow, thus separated from the Earth shadow, which was often very obscure.* The dark centre, 10° radius, showed the sky-tints above the counterglow. The rose reached 10° to 14° further occasionally being rayed, as on December 22, 1883, when one streamer nearly reached the zenith ; and on September 13, 1884, when the bow itself was ill-defined. In its inception the counter- bow resembles a gigantesque railway chair. / , //■ / II SVaS'^V \%. T -52 AM M'B.BYO. \SB'v.\.M.a ^l^^^. Cmvr\t.'RCV^\N III ^[dmmiMJ// \««'^\■^^^a••2.^.^^\. tDPlED BY YORK SEEK 81 L H\t«™sim \a3'i V\'tX ?ft 'See^j. 1-4, il B to 4k CO to »& r-1 UT «0 GO h^ Oi-i CTif^'-'UCO CdCiStOiO DSOVOCOO C« CO 1*.- CO *■ -^ CO CO CO M) <:o >l^ ^ Qo 8IO tst CO Jig OUiCX)^! rf^ri^QOC i-i ftO to CO--Z: a: tOQigO csoT Ul OS :0 3oS So 'l Q ^ w i § S 3^ 5J w > -, tuO ►< c CD Ms O 11 U5 53 Z o Co o r o S IS f^ s S ~ CO 42 About 30 minutes_after sunset, the counterbow rapidly vanished, usually soon followed by the counterglow. At the culminating moment, however, traces of rose began to appear above the point of sunset. Some time before sunset the rose of "Bishop's Ring," disappeared, leaving the "glory" to form a cone of brilliant, silvery light, enclosed bv sunset greens, shading into the ordinary twilight-indigo. The main glow began by the summit of this cone becoming suffused with deUcate rose tints. These extended rapidly, especially upwards, there merging into violet, and, the zenith being reached, " imperial purples." The sky beyond assumed the richest indigo shades ; whilst Venus and the moon assumed exquisite complementary blue-greens. A very important accompaniment, especially of the richest displays, was the appearance, just before sunset, of the filmiest of clouds. "To me the glare never seemed as if reflected from cirri ; it was much more like that from the smoke-originated clouds of manufacturing districts." They often showed faintly-marked striae, frequently running from S. S. E. to N. N. W. The glow was " blotchy " when most intense, thus indicating their presence. Sometimes, especially in September, 1884, and in midsummer, 1885, dark bands divided the glow, often cutting it off abruptly, especially on the north side.* So early as November 26th, at Street, Somerset, the writer's father observed " rays of the pink light shooting up from behind the cloud in which the sun was setting, like those of an aurora." ( r"-:( (Repeated at Sunset.) SUNRISE-GLOW, 1884 IX 13th. While thus developing upwards, an exquisite green spread out below. This seemed to extend slightly upwards, quickly followed by yellows along the horizon and these by orange, the green disappearing as the rose sank into them ; finally little but a lurid glow remained. But soon, though generally more than an hour from sunset, the afterglow occupied the position vacated by the glow, being much ruddier in tint. The brightest, coming about an hour and a half after sunset, resembled the glare from a tremendous conflagration below the horizon, and deceived experienced flremen. Whilst small print could be read, faint stars, as the Pleiades and Pons-Brooks comet, were visible through it. This reached a maximum in a very few minutes, and soon passed away, leaving a^lurid, *See lUustrationa, 43 From Notes.) COUNT ERGLOW, A. M., 1884, IX 13. SUNSET-GLOW (Street, Som.) 1885, VI 27. 44 fiery glare along the horizon, lasting even two aours and fifteen minutes from sunset. * Let us, next, briefly state and apply the explanations so excellently developed by Professor Kiessling.* He divides the normal sunset thus : Prelude : Silvery glistening of the western horizon. First .Act ; Sun enters this ; sets ; cone of light reaches up about 20° . Second Act : Tinges on clouds, first opposite sun ; blue to reddish- violet tinge on sky. Earth-shadow appears, surmounted by ruddy counterglow, which, 20 tc 25 minutes from sunset, suddenly disappears ; clouds to west brightly tinged. Third jict : Apex of cone glowing, shading off on all sides most gently, slowly sinking to mingle with yellow along horizon ; these to orange ; then lurid Occasional Epilogue : Very faint re-illumlnation. The whole he ascribes (p. 31) to diffraction through a very lofty stratum parallel to the Earth's surface, consisting of very uniform haze particles. Such a haze always accompanies a well-developed sunset. But the effect is neutralized unless the inferior layer is unusually transparent. Else it contains particles so greatly varying as to dissipate the diffracted rays. Such a layer will result from warm, moist air,+ the presence of which, accompanied by (except the last) brilliant ordinary sunsets, is shown by the table on the opposite page, condensed by the writer from Kiessling's extensive series in "Das Wetter" II, 9. The last one refers to the first German observations ol sunset phenomena. Hohenpeissenberg is 35 miles S. W. from Munich, both probably below the sky-region producing sunrise effects at Santis. The loftier stations accentuate the difference. Normally Munich should average 254 ° warmer thau Hohenpeissenberg. The following confirms independently the existence of such marked lines of contact. On December 25, 1883, the writer observed, at 2:45 p. m., a "ripple" of clear sky, J^'' to ?i° broad, traversing a beautifully marked, lofty cirrus abo\ ethe sun, traveling90° in 10 minutes, ending iO ° to 50 ° long. The cloud, as this passed along, melted entirely, except in its densest portions, which turned from opaque dark to transparent white. Evidently the crest of a lofty, warm wave penetrated right through the cirrus cloud, which was fringed with exquisite diffraction bands. CLOUD RIPPLE. 'A A, B. as First Seen. C. D. &c. Successive Positions. •*■ Set tabic, opponite. pagt. atsc * 'Daa Wetter, 1883 XI 1 23. • passim, especially 1 3 and II 0. 45 SUNSETS OBSERVED AT SllSTTIS (8200'), N. E. SWITZERLAND, DIFFERENCES OF TEMPERATURE, At HOHENPEISSENBERQ, (altitude 3,300 feet, [994 metres]) compared with Munich, (altitude 1750 feet, [528].) DATE OF SUNSET, 1 other stations than )■ Upper line grives date ; lower, difference of temperature in °C. Hohenpeissenberg. 1883, January 30th, - - 28th, 29th, 80th, 31st, —3-6 + 27 +4-3 — 2-6 " February 11th, 10th, 11th, 12th, 13th, 14th, —2-0 +8-2 +0-1 +6-1 +0-7 " April 27th, 38th, - 25th, 26th, 27t/h 28th, 29th, (Slight). — 4-9 —2-1 +1-2 +2-9 +0-7 May 5th, 1883, 3rd, 4th, 5th, 6th, 7th, —3-4 —1-7 —4-5 —4-1 — 3-5 But on Rigi, 5950', —10-4 -8-8 —7-7 —8-5 -8-6 Santis, 8300/, —14-1 —13-4 — 13 1 —11-3 —12-1 St. Bemhard, —14-7 —14-4 —18-6 —13-6 —11-4 1883, September 20th, 18th, 19th, 20th, 2l8t, 22d, —3-8 —0-9 +5-5 —20 -0-2 Rigi, —7-6 —5-7 + 1-2 -6-5 —7-0 " Oct. 9th and llili, - 7th, 8lh, mh. 10th, 11th, 12th, 13th, —1-9 + 1-4 +0-3 +1-7 +6-5 +3-0 -1-5 • ' Nov. 32d and 2ad, - 2lst, 2^(1. 23d, 24th, +0-6 + 16 + 4-4 —2-5 " I^ov. 29ih and 30th, - 27th, 28th, •^9th, 30th, Deo. 1, 2d, +0-8 —36 —1-6 +2-6 +5-2 — 8-4 Santis, —7-5 —9-9 —4-3 +33 -0-7 -9-7 46 The writer has not yet been able to obtain stations to associate with York in making comparisons similar to Kiessling's tables. Perhaps Fort "William and the summit of Ben Nevis would be most satisfactory. A careful exam- ination of local meteorological conditions indicates the absence of any promi- nent CO- variation ; but some minor agreements are exhibited in the table on opposite page. Professor Kiessling finds experimentally that the greatest deviation for red rays from a fine haze layer, forms a cone with an angle of 25° to 30° to the sun's rays, (as angle S B C in diagram below.) The chief effect may therefore be expected at this angle. Within it the rays, he says, meet with particles so varying as to re-combine the diffraction colors. But is it not rather due to the rays striking the haze at such varying angles ? For, at the given distance, they fall tangentially over a vast area of identical particles, thus causing similar diffraction. The disappearance of " Bishop's Ring " as the sun approaches the horizon, shows how easily the glow becomes obscured. This is partly due to absorp- tion, but chiefly to the same irregular diffraction which turns the day- glow tawny along the horizon, as seen at York. Only as the direct rays of the sun leave these lower, larger, unequal particles can the sunset glow be seen. The rose or violet tints never appeared within 5 ° of the horizon, where the silvery green changed only to yellow, orange, and lurid red. The "imperial purple " appeared only high up, usually at or beyond the zenith. The rays were doubtless due to clouds, as a rule below the horizon, inter- cepting the original rays. But dark bars were recorded from visible clouds in November, 1883.* In October, 1885, such a bar was observed shifting its position. The Counterglow is due to reflection from the very mist particles which obscure the glow itself. The diffracted rays, striking such particles at or near the line of the Earth-shadow, are reflected along their return course among unilluminated particles, thus suffering less obscuration, the more so that these lower layers have, of course, a much greater number of particles. I- BASED UPON KIESSLING'S " DAMMERUNGSBKSCHBINUNGBN," p. 33. ■S 7f^ Explanation. H B Surface of Earth. G H K Bay tangential to © at H. B L, M diffracted rays, striking tbe lower haze-surface, Y Z, at L & M : G K at X & J ; e at & P. L D, M F, the same rays reflected, part passing off along D U, B V. Q B Seat of afterglow. W X Y Z Haze cloud II to ©. A B C P Parallel ray, tangential to upper haze-surface. IJ seat of counterglow to persons B of O. P Seat of glow, cirri relit. D ^, E i", 2nd Internal reflection of L D, M E, striking © at Q & B. Clouds lit up 3rd time, (as Sept 12th, 1884). M B causes the wry prolonged red glare along horizon. LETTERS UNDERLINED INDICATE ADDITIONS. * Fide supra, p. 4, + See explanatory^ dififiram, above ; also, as rays nearer I tlmn J are reflected at a relatively higher ajigle, these, being iictirerthe earth, are also more obscured; compare c ose of paragraph. 47 S a E. ^ o £■ 1^ g g^ B B- :S o c 'i 2 o g o iS H. L- S ■o '^ '^ r« •TI i-b so O O o* W "■ o CT *<* CD "* B 5 >-: o c •*g 3 o g-o ^ p p to a =* tc 1-3 9? o EJ CO to m r* ^ " - S o s giving uble of cble tbi H- co + CO s s e:- H w ^ i S.~ value l),and , of (1 o *<1 i 1 T' ^ lo (+). ^ 109 CO o - g o None. K ! ^ 1— > ts ^ Slight (un- 3 > O rf^ CO CO ^"^ o der .05). CO CI to o -3 to *1 Strong (over .05"). 1 . g CO h-- 00 1-1 OI 00 None. a ^ CO to S. 1-1 g H^ H-1 Slighter'). S > o zo 60 CT CO o CO Strong (3-5). • — ,~^ 1 o 9 48 The CouNTEBBOW, the writer believes, no one has yet explained. Is the light from the region of maximum diffraction so concentrated that, on haze particles just above the Earth-shadow, a fogbow results ? This would be cut off sharp by the Earth-shadow ; meanwhile the wider-scattered glow would be reflected as a long, narrow band separating the bow from the Earth-, shadow. A feeble glow is preceded only by the counterglow. Again, the top of the bow comes last alter sunset, because its rays, after the internal xefleotiou and refraction, are more absorbed than those at the base of the bow, because tjiey have to traverse a greater thickness of illuminated haze. On December 22, 1883,* and September 13, 1884, (a. m.) the oounterbow and counterglow, respectively, were observed rayed obscurely, the latter time with 9 bars, against 19 noted 5 minutes earlier in the glow, but broader. No doubt only the higher, central parts were seen reflected. Finally the Foreglow and Afterglow Prof. Kiessling ascribes to simple reflection of the sunlight essential for the principal glow. For this thelofty diffracting cloud-haze requires a mirror-like surface. Such he proves experi- mentally possible, but without explaining the manner in which it acts. Possibly the rays are internally reflected at the lower surface and again at the upper, part emerging after this second reflection at nearly the same general angle and therefore the same center of brightness. As the diagram indicates, however, the same curvature which brings the afterglow so quickly after the glow, brings its centre rather higher. The diagram also shows how, with a thin haze-cloud, the two may coalesce. The more brilliant the glow the later, always, was the maximum, as well as first appearance of the Afterglow. Assuming the time of maximum to come when the solar rays strike the upper surface of the cloud-haze tangentially, then, whatever the height of the under surface, say 15 or 25 miles, the height of the upper surface must be measured by the time of maximum glow. Hence the brightest glows were also the latest, coming as much as 80 minutes after sunset, (December 1, 1883,) whereas faiut glows were only 20 minutes, (March 1, 1884,) (October?, 1885,) and once only 10 minutes (June 29-30, 1885,) from sunset. Of the fewer recorded morning glows, the latest was 44 minutes, (January 12, 1884, ) the least, 23 minutes, (April 13, 1884,) the evening interval next day being also 23 minutes. Faint glows begin, also, much earlier, because intensity will vary as thickness and the lower parts of a thick haze, tending to consist of larger particles, would neutralize the earlier glow on the upper parts. With a thin haze-cloud these layers become themselves the diffracting strata. An interesting transition from the ordinary diffracted effect on cirri, to that of the glows, occurred in December, 1884. On the 11th, at York, two small clouds were affected ; on the 13th it appeared as a fringe to a long, dark, very lofty haze-cloud averaging 18 ° above the S. S. W. to N. W., the colors occasionally thrice repeated. Above this, the haze was translucent with a second similar fringe. Thirty-five minutes after sunset, the dark cloud became violet, the translucent, steel-blue, both finally melting away, but reappearing later, the translucent band of a strong twilight white. This cloud was also observed widely over N. W. Europe. Telescopic definition has of late been unusually poor, a strong argu- ment for the constant presence of the haze-cloud, though so often non- apparent. If the basis is volcanic dust, then the opacity may vary greatly, as much or little moisture condenses around the particles. The relative humidity, also, may have been appreciably increased by the vast volumes of steam shot into these lofty regions. Accepting that the color effects spread from Krakatoa, first westwards along the equator, some 2,000 miles per day, and then towards the temperate zones, the following are the main facts : *Obs6rvaUon reported to w-Hter by L. Jiichards&n, Newcastle on Tyne. •i9 Krakatoa, after 200 years quiescence, suddenly burst into ei-uption, May 20, 1883; the explosions were heard over 160 miles away, and the ashes ascended four miles. A period of awful eruptions began on August 26tn, lasting some 36 hours. Half the island disappeared, leaving an enormous gull, two chief masses forming fresh islands five and seven miles off ; the whole region shrouded in pit<'hy darkness, raining ashes and pumice, lit up by volcanic and electric glaiv. Batavia, distant 93 English miles, was in darkness 36 hours, the air- wave putting out all gases at 1 A. M. The height to which matter was ejected can only be estimated.* The sound was heard at Seychelles and Mauritius, distant 3,000 miles ; sear-waves were registered the world over ; air- waves circled three to five times round. + Sound and height of projection both varying as squares, we may con- sider that, as the sound in August reached nearly twenty times further than in May, the height of eighty miles is, a priori, probable. For the finest dust this might well reach o?ie hundred miles : 1. From the constant uprush of erupted matter. 2. Prom much reduced air-resistance above four miles. 3. From the uprush of the Trades (resulting in the surface equatorial calms). 4. From the consequent immense expansion of the gases; which must also increase the velocity of their outward fiow. Assuming as probable this altitude of 100 miles, the "lagging behind" of the Earth's surface in comparison, as the writer noticed on January 14, 1884, would amount to 630 miles per day. Add to this the Equatorial com- ponent of the ascended Trades, accelerated as explained above,* and the immense daily velocity is well accounted for, even disregarding the proba- ble effect of electric repulsion. § The meridianal component of the Trades, ( i. e. the portion of their veloc- ity measured at right angles to the Equator,) the south being in excess of the north, explains why higher northern latitudes were attained at each revolution of the dust cloud than southern. Hardly sufficient attention has been paid to the extreme comparative prolongation of twilight in Equatorial regions compared with temperate. This also supports the view that the initial height was enormous, the down- ward flow of the upper currents doubtless reducing it In Temperate Zones. Perhaps, accepting the above explanation of the afterglow, it would not much exceed 25 miles, reckoning by the maximum glow ; for the brightest occurred when the sun was only 9 ° or 10 ° below the York horizon. The final glare lasted, December 1, 1883, until it was 16 ° below. The European records, and perhaps, also, those of the Northern United States, indicate plainly that the glows struck the continent from the S. W. Mr. Ringwood suggests that this was due to the Aleutian eruption. II Such a coincidence seems so unlikely that it is more natural to consider that the return S. W. Trades gave their direction to the dust-flow in these higher latitudes. The preceding pages, after giving the result of personal observations, attempt to elucidate some less prominent features. The connection of the glows with Krakatoa and with ordinary sunsets is treated as hardly requir- ing further confirmation. '»~Dust, ona inch deep, fell on, a ship 970 miles E. ^ S. of Java UeaiUNatwe. 1«83, DeclSth.) t See Nature, July 17»i, and Science. Aug. 15, 1884. t See, also, Mr. Bingviood' s paper, givmg observed velocities, Nature XXX. i>. 301. I Nature, XXIX, p. 180. I Nature, XXX, p. 301. 50 The great secret of the whole phenomenon lies in the elevated haze-layer; diffraction by this produces " Bishop's Ring " and the first glow ; further re- flection, the Fore and Afterglow and Counterglow ; and additional refraction, the Counterbow. Incidentally, the cloud re-illuminations, preceding the Glow and Afterglow, are likewise explained. Thus the diverse problems require but a single clue, presenting us with a unity which gives the argu- ments an aaditional and peculiar cogency to those who havefelt bewildered by the vastness, the novelty and variety of the magnificent spectacles dis- played upon the l.eavens during recent years. tt H H (> tJ g O ^ 5 .0- p- no P* 1 1^ Q B ^ B 00 (0 o s' 2" s ■< K a ^ 51 a m S t=l : p- B <£. c :^ (T P 3 W? [ft! ^ 1 1885— York, Nov.15-19 Nov. 28, Deo. 17. ... At Street— 1885, Dee. 23, to 1886, Jan. 11. York— Feb. 4th (107 78 66) (104) 80 50 c Finest, g o Ends. ^ 00 -.D li £ g CO ^^ o w Beenis. O Finest, o End*. 1 o d :t 5 CO Begins, c Finest. £ s finds. 2 -5 JO 00 jj _2 5 :; -Id Beg int.. a Finest, o BjkJs. s^ ri CO c ^ ^ ^ \ PLrii..i: > "-H The "Red Light." By henry C. MAINE, Eochksteb, N. Y. rE appearance of what are known as the Red Sunsets or Red Light, in the autumn of 1883, is regarded as one of the most remarkahle meteor- ological events of modern times. The strange feature of the Red Light was its long duration after sunset, and a peculiar halo or corona about the sun by day. The light after sunset was usually of an orange red or a rose color, and reached far up toward the zeuith in the form of an arch, with a bright spot at the highest point. There was also a bright spot and colored arch in the Bast, opposite the sunset point, as if produced by reflection. The horizon to the North and South was also lighted with red until a late hour, sometimes 9 o'clock. On a few occasions the light assumed the form of alternate sectors of rose colored light and blue sky, with auroral action in the colored streamers. One of the most interestiug exhibitions of the kind was upon the 19th of September, 1885. At nearly every exhibition, when the rose color was prominent, auroral action could be detected. The phenom- ena of the sunsets changed rapidly, arch succeeamg arch with changing col- ors as the sun went lower and lower. The halo by day had an ashen or salmon tint on the outer border, which shaded into the sky. The border was irregular, being extended in various directions at different times. (See photograph No. 3. ) The ordinary ring or halo about the sun has edges well defined, with more or less display of prismatic colors. (See photograph No. 3.) The first step in determining the cause of the halo and vinusual prolonga- tion of sunset effects was to ascertain if they corresponded in time and intensity with other phenomena, and then determine the probability of phys- ical connection. When the Red Light appeared, the sun was near its maxi- mum of activity or spottedness, and the earth had been vexed with the most violent storms, and floods had been very destructive. Having observed the sun daily, since the .solar activity began to increase after the minimum of 1878-9, with the result of noting a correspondence in time of the most ter- rific storms on the earth with similar disturbances on the sun, observation was extended to the Red Light. A brief record of the most prominent sun- set displays must sufBce : There was great solar disturbance at the time the green suns and red sun- sets appeared in the equatorial belt, in the beginning of September, 1883. The green suns were seen at Panama on September 3 and at Trinidad on the same date. On the first of September twenty new solar spots appeared, and on that date there were seven groups and ninety-five spots, one of which was visible to the naked eye. There were cyclones of great energy in the equatori.al seas at t'.ie time, and the captain of a dismasted vessel was one of 54 NO. 1.— THE ROSE COLORED ARCH AT SUNSET. The rosy sunset of November 22, 1885, photographed by Henry C. Maine, showing the rttosy arch and the brilliant light below it near the sun. NO. 2.— THE SOLAR CORONA. The Red Light corona or halo about the sun, photographed by Henry C. Maine, at noon November 22, I885,_ The vapors near the horizon are also lighted and of considerable actinic energy. The salmon color is in the faint outer haze surroundingthe central brightness. the first observers of the strange light in the sky. The Red Light appeared in Western New York on November 34, 1883, after a severe storm had passed over the great lakes. There was great solar disturbance at the time and the light was at a maximum on the 27th. On that day, the ashen halo men- tioned above was very conspicuous. This persisted with slight changes for more than a year. On the second of December the Red Light was not seen in Rochester, and the sun was nearly clear of spots. A number of new spots appeared on the 6th, and on the 8th the Red Light re-appeared. It brightened until the 10th, when it was very brilliant. The Red Light faded as the sun storms disappeared by the sun's rotation. December Zlst a spot area of large extent appeared, followed by great meteorological disturbance, and the Red Iiight shone again, reaching great brilliancy on the )iGth of December. This maximum was also noted by Dr. F. A. Forel, at Merges, Switzerland. The light waned until January 1st, when there was an ordinary sunset. On Jan- uary 3ud active sun storms appeared and on the 3d, after an electric storm which drove telephone operators from their instraments in some places, the Red Light re-appeared. After a great storm, the light was brilliant January Sth and morning of the 10th. On the 17th the light was brilliant, following new solar storms. On January 25th the light was very bright, following a great chain of sun storms. Hurricanes occurred in England on the 22nd and in France and England on the 26th. The Red Light then decreased in bright- ness. On the 11th of February active sun storms re-appeared ; tornadoes occurred in the South on the 13th and the Red Light was noted on the 14th. On the 19th two new sun storms came, .the Red Light increased, and six southern states were swept by tornadoes. The sky was of a lurid Ted at midnight, probably from electric action upon vapors of the atmos- phere. A new sun storm came February 24th, and the light continued brilliant, but faded in a few days. [The greatest Ijrilliancy of Red Light, and severest terrestrial storms were noted when sun spots were between the eastern limb and the sun's meridian.] On March 2nd, 5th and 6th, new sua storms appeared and the light shone brightly. A destructive general storm followed. More sun storms came on the 13th and 14th and the Red Light was at a maximum on the 17th. Then there was a descent toward a minimum. March 2.5th, a sun storm developed on the sun's disc ; tornadoes swept seven states. The sun storm developed the largest group of spots seen up to that date. The Red Light shone with remarkable brilliancy on March 27th. April 1st a great chain of sun spots appeared ; tornadoes followed in five states and on the 5th the Bed Light was intense. Thus the light fluctuated through the entire spring and summer of 1884. In the autumn of that year the skies wei e very brilliant at intervals, always corresponding with the intensity of solar action. In the late winter and spring of 1885, the sun storms began to diminish, the Red Light nearly disap- peared and the peculiar halo about the sun was no longer conspicuous. Toward the middle of May there was a marked renewal of the solar storms and by the 1st of June the spots were very numerous and large. During June the sun was the seat of convulsions of the most remarkable character, (see photographs of June 20th and other dates,) accompanied "by a long series of very destructive storms in all parts of the world. Early in July the Red Light re-appeared. On the 5th it was seen in Rochester, and in Oregon* two days earlier. On the 31st of July the bril- liancy of the Red Light reached a climax. Thebright rose colored spot above the sunset point again lighted objects like a second sunset, and appeared self luminous. *The 'Western sky was colored a bright roseate hue last eveninsr and all around the liorizon and up to the zenith ^he clouds were fringed with red, a repetition of the red fiunspts of last summer This is the first time the phenomenon has been seen in any degree of magnitude th-is season.— PortlaTMi Morning Oregonian, July 4, 1S8S. NO 3 -PRISMATIC CIRCLE OR HALO. Halo of water vapor at a low altitude, photographed by Her,ry C. Maine, on Nov. 20th. 1885, a few days previous to a great coast storm. NO. 4..-GREAT GROUP OF SUN SPOTS. The sun. June 18th 1885, photographed by Henry C. Maine, 57 The sunsets at this date were, as I observed, mostly of a rose color, which varied iu iut(3nsity. They continued with varying brilliancy through August. The halo about the sun had re-ai^ijeared as a white corona, which increased iu density until the salmon color on the outer border was noted again on the 2ud of September as very conspicuous, as was also the Red Light. The halo still persists a,nd was quite brilliant on the day of the annexed photograph, November 32, 1885. By reference to the records of the Signal Service, it is noted that the Red Light varied in intensity at different places on the samedate, showing oouclusively that local conditions must have had a part in producing the phenomena. The best observers reporting to the Signal Service noted the difference between the orange* and rosy sunsets. The Red Light continued during September with the usual fluctuationst, being very brilliant on the 14th, and some days thereafter, following a great solar disturbance preceding the Washington Court House tornado. These observations show that these phenomena, great storms on the sun, extended and severe meteorological disturbance on the earth, and the red sunsets, corresponded in time and intensity. The fluctuations of the Red Light also corresponded with the periods of change in solar agitation+t. la there a fair presumption of a physical connection ? The persistence of the peculiai' halo about the sun for more than a year, while the red sunsets were very unequal, sometimes disappearing altogether, indicates that there must beseveralfactors to produce the sunset phenom- ena. Some of these factors were less changeable than the others. The halo showed but little change for a long period, although it was noted that on most occasions the Red Light was brilliant at night, when the halo was most conspicuous. What was the condition of things which rendered the halo persistent while the sunsets changed, almost wholly disappearing at intervals 1 A terrific volcanic eruption in the straits of Sunda, Island of Java, on the 26th of August, 1883, has been regarded by many as the cause of the red sunsets. It has been held that the dust from the crater spread over the whole atmosphere of the globe at a great height, reflecting back the sun- light, after the sun had set, for a greater length of time than was usual. If the medium of reflection were dust suspended permanently in the atmos- phere ; and if the dust caused the solar halo, the presence of the halo about the sun by day ought to prove the presence of the dust, and the red sunsets, which are supposed to have been dependent on that dust, should therefore have been uniform during the time the halo was visible. But the sunsets were not uniform during that period, as has already been shown. This does not, however, wholly exclude the dust as a possible factor. But it is difficult to conceive how dust could remain iu suspension at so great a height for more than a vear, then disapi>earingfor a timeand returning again last July and August. To explain the long suspension of the dust, those who adhere to the "dust theory" have assumed that it may be mingled with water vapor at a great height. Judging from observation, and the remarkable localization of the red sunsets on many occasions, as before noted, water vapor must be considered a very important factor in their display. The *Vevay, Indiana : Yellow or oraug-e sunsets wore observed on the 1st, 5th, 13th, 15th, 17th 30th, 28th and 30th. Bosy sunsets were observed ontheSd, 8th, 9th, 10th aiidl6tli. — Signal Service Monthly Weather Beviewfor Auyust, 188S. +The color of the skies after sunset again deserves note. Many observers record especial colorinsj, on dates from the 18th to the end of the month. The colors are vari- ously described as oi-anso, crimson and Ti>inli.~— Bulletin of New England MeteoroUjgi- cal Society for September, 1885. ttM. Faye says: "It is what may easily happen in the progress of a periodic phe- nomenon which passes rapidly, and without fluctuation,*frora a minimum to the fol- lowing maximum, but which passes slowly, bv n sorios of secondary oscillations, from the maximum to the following" minimuiu. This is in ollect, the well-known progress of solar spots." 68 NO. 5. -ACTINIC ENERGY ABOUT A SOLAR STORM. The sun, June 20th, 1885, at noon, photographed by Henry C. Maine. The great group spots wasabout 110,000 miles long. The aotinio enefgy in the region about the sun storm IS so intensethat other parts of the sun are left in shadow. Upon the 20th destructive irms swept the Northern States. maiuteuaiicoof Will (■!■ vapor at a height suflloient to reflect or refract the light of the sun after it is twenty degrees below the horizon, a distance which has been calculated by Mr. Serviss and others, requires unusual conditions. Where shall the conditions be sought? Do they exist in the eartli itself or its atmosphere? Evidently they do not. Then they must be sought outside, and can be found , nowhere except in the sun. The sun's intense activity during the past five years supplies all of the conditions necessary to raise the vapor, by added heat and electrical action, to an abnormal height. But the same condition of the sun which would elevate the vapor to a great height, would also greatly increase evaporation from the waters of the globe, and give rise to excessive rainfall. As a matter of fact, such rainfalls have occurred and are now occurring. Proceeding a, little farther, it will appear that a condition of the sun which would produce the effects noted, must also have some appreciable effect upon the sun itself and its immediate surroundings or vaporous envel- ope. In an annexed photograph (No. 6) of the sun, June 12th, 1885, will be seen a luminous cloud of enormous dimensions, apparently floating high above the sun's surface, for it is brighter than the sun itself. This matter, (probably blazing hydrogen,) if it does not pass out among the worlds of the solar system, goes to increase the nebulous, matter about the sun. During the extended maximum of solar activity, (which has been stretched out two or three years beyond the ordinary limit,) this matter has passed out almost continually into the vapor envelope of the sun, as smolie and vapor rise In our atmosphere. But this sun vapor rises with much greater velocity from the sun, as the attraction of the sun is greater than that of the earth. The great increase of the eruptions of sun vapor during the present sun- spot maximum, would enormously extend the vapor shell about the sun. If the earth is involved in an envelope of its own dust thrown to an unusual height by the Java volcano, as the " dust theorists " claim, how much more must we expect the sun to be involved in its own vapors, since the activity there exceeds by a million or more times the feeble efforts of a world cooled sufficiently to be inhabitable. The sun has the reputation of being a nebulous star. Tennyson says in " The Princess " ■- "There sinks the nebulous star we call the sun. If that hypothesis of theirs be sound." Nearly -very astronomer who has observed the sun has observed the passage of vast, luminous vapor clouds, mostly hydrogen, into the sun's atmosphere, or away from the globe of the sun. Professor Young saw such an event in 1871 and recorded it. The cloud rose to the height of two hundred thousand miles from the edge of the sun, at the rate of 167 miles a second, before it faded from view in the spectroscope. Professor Young calculated that the first outburst of this vapor must have been at the rate of at least 300 miles each second. Louis Trouvelot, at Meudon, near Paris, saw a mass of luminous cloud move out from the sun on the 16th of August, 1885. The observers at New Zealand of the total eclipse of the sun, September 9th, 1885, saw with the naked eye a red flame shoot out near a rift of the corona. So far as known, no such vapor cloud was ever photographed until last June, except during a total eclipse. Professor Young said in his address before the American Association for the Advancement of Science, at Philadelphia, in 1884 : "As regards the actual existence of an extensive gaseous envelope around the sun, it may be added that other appearances than those seen at an eclipseseem to demonstrate it beyond question — phenomena such as the original formation of clouds of incandescent hydrogen at high elevations and the forms and motions of the loftiest prominences." Besides the reasons already stated for believing the sun's vaporous envelope is enormously extended during great solar activity, thereis another which is most persilasive, and which explains a puzzling matter in areasoua- NO. 6.-HYDROGEN CLOUD. The sun, June 12th, at noon, 1885, photographed by Henry C. Maine, showing luminous cloud of hydrogen. 61 ble way. That matter is the peculiar retardation of Enoke's comet during certain of its perihelion passages, and absence of retardation at other passages. Professor Simon Newoomb says in his Popular Astronomy : "Dr. Von Asten found that between 1861 and 1865 there must have been a retarding action like that supposed by Enoke. Carrying his work forward to 1875, he found that between 1871 and 1875 there was once more evidence of a retardation, about two-thirds as great as that found by Enoke. The absence of such an action between 1865 and 1871, therefore, seems quite exceptional and difflcult of explanation.'' It will be seen by reference to the past records of solar activity that the years of retardation were years during or imnaediately following maximum solar disturbance. The comet was probably retarded then because the solar envelope was greatly extended ; and the comet had to move through the vapors thus sent out into space by the eruptions below. When the solar activity in a measure subsided, toward the minimum period, the vapor thus thrown out condensed and returned to the sun or was dissipated in space. So the comet would meet with less resistance upon another return. It was the opinion of SiT William Siemens that the matter thrown out from the siin's equatorial regions passed out beyond the earth's orbit and returned again by re-ourving to the sun's poles. If this theory is true, more matter would pass out from the sun during maximum solar activity than at other times. ' Bearing all these facts and theories in mind, is it not probable that the violent solar eruptions during the past five years have so loaded and extended the solar envelope that the nebulosity has become visible, and that the visibil- ity began in the autumn of 1883 ? The effects of the solar eruptions upon our atmosphere might have been such as to aid in rendering the sun's envelope visible through vapor at an abnormal height. Such conditions explain the persistence of the solar halo, and its changes in form, while the sunset phe- nomena which depended partly upon local atmospheric conditions, varied from day to day. The halo or corona about the sun itself may have been exaggerated to our view, greatly beyond the actual limits of the solar envel- ope, by the condition of our atmosphere. Indeed, part of the display must be atmospheric. Suppose an extension sufficient to retard Encke's comet, which had a perihelion distance of about 30,000,000 miles, and it will not be far from the corona, which persisted from November 24th, 1883, for more than a year, and is still seen at intervals after great solar activity, and meteor- ological disturbance on the earth. But the corona of the present maxi- mum period must be much greater than the coronas which were encoun- tered by the comet on the dates mentioned by Dr. Von Asten. Given this corona or envelope with sufficient density towardlts outer edge to reflect the sunlight, and we have the rose colored arch, with its bright spot, which followed the sinking of the sun, with the brilliant reflection in the East; also the sunrise eSeots which were quite as notable. Given this corona, and the character of the sunset would change from day to day through the changing condition of the vapor and possibly volcanic dust in our atmosphere. When the atmosphere wa-s heavily laden with vapor and possibly dust from Krakatoa, the arch would be lost in the orange red glow of the gorgeous sunsets, as on November 27th, 1883, and later dates. When the dust had settled, if it was ever in our atmosphere, at the latitudeof New Tork the rosy arch would persist as it did and the corona would also remain by day. The arch lighted the dust and watery vapor and the image of the arch was projected on our atmosphere ; but when both dust and vapor were at a minimum, the arch alone was seen, with a faint rose color. This color is the one that might be expected from the character of the vapor, mostly hydrogen, in the sun's envelope or corona. Prof. C. A. Young says in his work on the sun, page 207 : ' • Tiie observa- tions of the eclipse of 1871 by Lockyer and others show that hydrogen in a 02 feebly luminous condition is found all around the sun, and at a very great altitude — far above the ordinary range of prominences. " This observatiott was near the sun spot maximum, and this accounts for the success of the observation, when luminous hydrogen was not observed at other eclipses. The slightly varying brilUancy of the rosy arch, and of the halo by day is accountedfor by the varying energy of the solar eruptions, the condition of the sun changing the condition of the envelope about It, and also affecting the earth's atmosphere. The auroral action of the Red Light is also dependent upon the solar condition. With the corona receiving and reflecting the sunlight after the sun had set, it is not necessary to conceive that the water vapor was raised to so great a height as to reflect the sunlight after the sun was twenty degrees below the horizon. But the vapor must have been elevated considerably, as the condition of the sun and the excessive evaporation would warrant this. But such ,elevatiou to fit any theory must depend upon the sun and its increased activity. The duration of the Red Light after sundown was varied by the varying height and density of the water vapor or dust, which were dependent upon meteorological conditions. Prof Balfour Stewart, the eminent director of the Kew Observatory, says that "the magnetical and meteorological processes of the earth are most pronounced when there are most sun spots." The intensifying of terrestrial meteorology has been so pronounced during the past five years that no argu- ment is necessary here. The record of the tornadoes, cyclones and floods is a part of the history of those years, and is spread out ev^ery wherein the daily press. From all these considerations it would seem that there is a reasonable presumption of a physical connection between the unusual solar activity and the Red Light, and that the one is the principal cause of the other. ADDENDUM. January 4, 1886. Db. Swift : Dear Sir : My attention has just been called to the following from the Scientific American of the 3d of January, 1886. I presume it had not before bcpn published in this country; and appearing a month subsequently to the date of my essay in which the same views of the corona were independ- ently advanced, it should not interfere with my claim to original treatment. I trust that you will submit this note with accompanying extract as an addendum to the essay of "Obsbkver." THE CORONA VISIBLE TO THE NAKED EYE ON HIGH MOUNTAINS. Scientific American, Jan. 1, 1886. Professor Tacchini, a great authority among scientists, gives a remarka- ble piece of information in a letter to L' Astronomic. He records that M. JPavel asserts that on high mountains, when the sky is serene, the solar corona is so apparent that it strikes all observers. The mountaineers and dwellers among the Alps agree in affirming that the phenomena is some- thing entirely new. Tacchini also gives an experience of his own on the subject. He made the ascent of M.t. Etna in July last. When near the volcano, at a height of ovor 10,000 feet, under a clear sky of a dark blue tint, he saw the sun surrounded by a white aureola, concentric with a magnifi- cent corona of a coppery red. The corona was transformed nea;r the hori- zon into an are less defined and of much greater extent. The origin of the Red Glows. Uv Rev. SEREXO E. BISHOP. Honolulu, Hawaiian Islands. THESE brilliant phenomena first began to be observed on the 28th day of August, 1883. They have continued with varying but diminishing^ intensity lor more than two years. They first appeared in great splen- dor plong an Equatorial belt of 18,000 miles or more. They gradually extended with reduced brilliancy to the Temperate zones, exciting the wonder of Europe and the United States in November, 1883. T^e most conspicuous of these phenomena take place during one hour or more before sunrise and after sunset. They may be considered as a great uitei'sifying and prolongatiou of common twilight sky reflections, in eonse- quen oe of a recent introduction into the higher regions of the atmosphere of some kind of fiuely divided matter which powerfully reflects the sun's rays, especially the red. The usual order of changes is as follows. Clouds not obscuring tlie view, the horizon where the sun has just set is occupied by a bright silvery luster. Above this to a height of 30° or 40° a. yellowish haze fills the Western sky. Although seemingly opaque and dense, the presence in it of Venus or the crescent moon show it to be entirely trans- parent. This haze rapidly changes in color and extent, ranging througli greenish yellow and olive to orange and deep scarlet. As the dusk advances, orange and olive tints flush out on all sides of the sky, especially in the East. The chief body of color gathers and deepens over the sunset, rapidly devel- oping the red. In from 20 to 30 minutes after sunset, deep scarlet has over- powered all other hues, flaming along 60° of horizon, and 10° of altitude. This rapidly sinks and intensifies. There is a dark interval above the red. The stars begin to appear. While yet the color flames low, above the dark: space appears a repetition of the orange and olive hues. Seen against the. ni-'ht-sky, these secondary reflections or after-glows are seemingly more bril- liant than the primary ones. Again the colors change and deepen into red, aud after the stars are all out, and the earlier flame has sunk below the hori- zon, and far later than any common twilight, a vast blood-red sheet covers, the West. It has been seen rising as high as 20° As it sinks and rests low on the horizon, in the dark night sky, it preciselv simulates the appearance of a remote and immense conflagration, for which it has in many places been mistaken. I have known our usual 30 minutes of twilight to be pro- lou'j:ed to 90, before the last glow disappeared. 64 In the dawn recur the same appearances, but in inverse order. In Sep- tember, 1883, they were singularly impressive and even terrific, as the first low sullen incandescence rose and spread and glared among the stars, as if the very heavens were in conflagration. Then, as well as at nightfall, a marked division occurs between the night-glow and that nearest to the sun. During the earlier weeks of the display, the dark interval was often extremely distinct. One observer (a) described it as a "black bow. " Another saw the shadow of the remote horizon sharply projected upon the under surface of the haze-canopy, but with fine >errations, probably the shadows of pla^ toons of cumuli L^J . Evidently at that early date the canopy of floating haze had a well-defined under-surface. From the beginning, the upper limit of the night-glow has always been indefinite, since its light was reflected to it from the broad surface of the first Glow, while the latter showed a clean shadow of the horizon from the sun itself. In general it may be said that the tropical displays of these Glows at their birth during the first week in September, as far surpassed the mild Glows seen world-wide iu November, as the plunging surges of a tempest surpass the tripping crests of a breeze. The entire dome of sky above and around seemed to heave with billows of lurid light, as the portentous masses of color poured out of the pellucid blue, while the West outflamed in broad conflagratioii.s. In September, during the day, as well as after sunset, many portions of the haze-canopy were noticeable as having a wavy or rippled structure, [cj A conspicuous object when the sun is high has been from the first the opal- escent silvery glow around the sun. This occupies a circle of 25° radius or more. The outer part develops a pinkish hue, which against the blue sky shows lilac or chocolate tints. These have a singular effect when seen through rifts of oloud, as Capt. Penhallo w [d I saw them on September 18th, 1,000 miles N. E. of Honolulu. This sun-glow has been particularly discussed by M. A, Cornu iu the Comptes Rendus, of September 23. 1884. He remarks peculiar modifications therein of the atmospheric polarization of the sun's rays. Prof. P. A. Porel has repeatedly discussed this sun-glow, which he has named Wi the "Cercle ue ±>ishop," after the first observer of the phenomenon at Hono- lulu. Prof. Huggins found this sun-glow putting an end to his previously successful photography of the Solar Corona. The height of the main body of this haze in the atmosphere has been variously estimated at from 15 to 40 miles. The present writer, as the result of much and early observation, has no doubt that in the early part of Sep- tember, 1883, no part of its under surface was less than 30 or 40 miles above the ground. All estimates should be based upon the first reflections and not upon the secondary glows. No decisive tests of the nature of this reflecting matter have been secured. The spectroscope has distinctly indicated the presence of large quantities of aqueous vapor, L/l accompanied by other peculiar influences. Fresh fallen rain and snow have repeatedly yielded a dust of microscopic particles possessing the same constitution as the flue ash- fall from Krakatoa. The most generally accepted theory of the source of this new matter in the sky, attributes it to the great eruption of the crater of Krakatoa or Kra^ katao in the Straits of Sunda on the 27th of August, 1883, one day before the flrst definite record of Ked Glows, which were seen on the 28th, at both Maur- itius and the Seychelles, 3,500 miles west of Krakatoa. Before considering the evidences in suport of this theory, notice needs to be taken of two other hypotheses, which have been advocated. One of these assumes the meeting of our globe with some cosmic cloud of impalpable dust, which was arrested in the upper strata of the atmosphere. a. Nattt/re, vol. 29, p. 549. 6. Nature, 29, 549. c. Nature, 29, 174. d. Natwre, 29, 174. e. ArclvVves des Sciences physiques et Natv/relles, tome 18, jt.465. /. C. Michie Smith, Nature 65 The other hypothesis supposes the oosmio oloud to have been oomposed of hydrogen, which united with the oxygen of the atmosphere to form th« aqueous vapor evidently constituting so considerable a part of this haze. The latter hypothesis seems open to the objection that such uniting of the two gases is usually attended with active combustion, none of which was observed. ^ Both hypotheses suffer from the total absence of evidence that any such cosmic cloud did approach the earth on or before August 28th, or since that time. The matter actually introduced into our atmosphere is brilliantly conspicuous in the sunlight. Yet we are asked to believe that a vast nebula of such matter approached, unseen and enveloped the earth. In 1861, the tail of an immense and brilliant comet actually swept the earth. Yet so ten- uous was the impinging matter that no traces of its presence were left behind. A cloud sufBciently dense to create the present haze, must in its approach have presented the aspect of a most compact and refulgent body. So far from being possibly unobserved, it must have terrified mankind. Another and most serious objection lies in the original narrow localization of this haze in an equatorial belt. It is difEioult to conceive of a cosmic oloud possessing a mass adequate to the immense effects produced, which should not occupy such dimensions as to completely envelop the globe at once, pro- ducing Glows simultaneously all over the earth, not to consider the improb- ability that the course of such a dense little nebula after collision should precisely coincide with the Equator. It must be remembered that stray oometary or nebulous matter (not solid meteors) afloat in oosmio space, since it possesses small mass and feeble centripetal force, necessarily assumes immense volume and extreme attenuation, compared with which this haze is solidity itself. The entire quantity of this peculiar matter actually dif- fused in our atmosphere, must originally have been equivalent to many cubic miles of solid matter, which represents a volume of cometary material immensely exceeding the dimensions of the largest planet. The actual local- ization of the first Glows in the Tropics thus precludes reference to cosmic sources, and compels us to seek a terrestrial one. Many have felt that the long protracted continuance of this haze in the air necessitates the supposition of renewed supplies from fresh sources, as if perhaps the earth were continuing to traverse successive regions of cosmic vapors, (which no one has seen). Had there been but one original introduc- tion of the haze, must it not long since have been precipitated and disap- peared ? But we have to consider how slow is the subsidence of even coarse common dust, especially in currents of air. The haze matter in question had probably 40 miles to fall. If only 20 miles or 105,600 feet, it must fall 144 feet in a day to reach the ground in two years. It seems improbable that these uitra^microsoopic particles could descend at one-tenth of such a velocity ? fsl It seems likely, on the cootrary, that the finer particles of this matter will continue suspended and produce their Glows for many years to come. Leaving these nebulous imaginings, let us pursue the plain, if humble, historical method of inquiry. When and where were these phenom- ena first observed? Under what peculiar conditions and with what attendant circumstances did they appear ? In what successions of time and place did they first occur, and to what actual point of origin on the earth's surface may they be traced ? Pursuing this indispensable method of physical investigation, we find that the earlier appearances of the sunset Glows, were as a rule immediately pre- ceded by a peculiar veiling and discoloration of the sun's disc, commonly termed the "Green Sun." While the sky was cloudless, or faintly obscured by vindefinable haze, the disc of the sun was described W as pallid, livid, bluish, ^ John Le CmU, Ncctmre, 39, 404. ft. Natwre. 28, pp- 576, S-TI-VolHS. w 88, 76, 138, 181, 649. fi6 coppery, greenish, " bird' s-egg hue," "plague-stricken." Itcouldbedireetly viewed with the naked eye, audits spots distinguished. At the altitude of ^° the sun generally resumed its ordinary aspect, but again turned pallid and green as it descended in the West. In some cases the sunset glares immediately succeeded, while in others they were not reported, the haze probably having been too dense for the sun's rays to penetrate it obliquely, so as to be reflected from its under surface. The first appearances of the Bed Glows were so intimately associated with the Green Suns that it is impossi- ble not to treat them as different aspects of one and the same phenomenon. It seems in place here to cite Mr. Whymper's observation Wl of Green Sun and wonderful Sky-Glows comijiued. On the third of July, 1880, on the upper slopes of Chimborazo, Mr. Whymper witnessed an eruption of Cota^ paxi, smoke from which drifted over the observer's position. Seen through it, the sun's disc assumed a peculiar green, while the changing colors of the sky "surpassed in vivid intensity the wildest effects of the most gorgeous sun- sets." From such records as were accessible, I have constructed the accompany- ing tabulated statement of the earlier recorded appearances of the Green Si.js and the Red Glows. The latitude and longitude of each locality are given in the table, with the date of the first appearance of the phenomenon at each point. The distance from Krakatoa is estimated in English miles, the number of hours in transit and the velocity of the current calculated. The source of information is specified for each of the seventeen different localities, three of which were on vessels at sea in the Pacific. To these, Mar- anham might be added. I lack the needed reference. At six of these locali- ties, both the Green Sun and the Red Glows were reported as having been seen on the same day. At four points only Red Glows were reported, and at seven only Green Suns. The most remarkable fact evidenced by this table is that the earliest appearances of these phenomena are thereby traced along a line of points, successive from Bast to West, lying very near the Equator, beginning at the Seychelles Islands in the Indian Ocean, and running thence in successive days through Cape Coast Castle, Trinidad, Panama, and Fanning's Island, arriving at Strong's Island on September 7th, having traversed a great circle for 17,600 miles in about 230 hours. It thus appears that the original haze cloud, which first produced the Red Glows, swept west from the Indian Ocean in an Equatorial Stream or Belt, which traversed more than two-thirds of the circumference of the globe at an average velocity of nearly eighty miles an hour. A precise estimate of its velocity between successive points is prevented by the imper- fection of the observations made. The date at Cape Coast Castle is uncertain by one day. The dates at Seychelles and Mauritius are probably vitiated by the copious diffusion of volcanic smoke prior to the regular movement of the upper stream. It seems quite clear, however, that an average velocity of about 90 miles an hour during the first half of the course of this haze- stream became reduced to about 60 miles in its later stages. These data appear to favor the conclusion of Mr. S. E. Bishop, D] that a stream of vapors was discharged over and upon the upper surface of the atmosphere of the Indian Ocean, by a powerful initial impulse, which drove it straight in a great circle, independently of atmospheric currents, and that this stream gradually suffered retardation as it descended into the atmos here, finally ceasing over the Caroline Islands. Without necessarily accepting this writer's theory, showing how such an impulse would be generated by the rotation of the earth, it seems clear at least, that the inception of the Equatorial Haze-stream, and its attendant Glows has been traced with positive certainty as far as the westgm side o£ i. Nabure, 29, p. 109. J. Hawaiian MontMii, April, 1884. 67 5? Q ^ o H a n hj w h3 o op fe a) M ^1 p CD g» E. B a I !z| « O) !z! !2! S! :z! 2! 3 !3 !? 71 CO CO 03 00 - - o o I qg ^ I I H B H &^ H ^ ^ ^ ^ ^ -q OS cn OI o O Hi (-1 W -5 Oi ^ ^ t? ^ ^ ^ ^ ^ ^ H M H c 0? S S g g If P" F F -^ ^ P4 CO s a s y .** !'' ?" s s s a >■ >■ J) J) ^ e a B s » _W I-' QD 00 00 00 "to 't^ Ifc. 00 00 'm 8 8 8 S S S -CI 03 CO ts to 00 00 *S g g g g ^ § g. p Q Q P P p P d p !p !p c £P CO CD !» CO 00 SB CO » i» CD s» CO J» ttf fd fd ^ Sd ftl 03 00 pD P'^ P° P° 00 QQ OQ I |S. -S P 3^-^CX}£!^gcn :3 g 68 the Indian Ocean, and back to the 28th day of August. Eastward of this, our search is arrested by a vast pall of volcanic smoke proceeding from the greatest eruption described in history. But if we stretch our line back through this obstructing veil, 30 hours in time and 3,500 miles in distance, we find ourselves confronted by the great final explosions of Krakatoa on the morning of August 37th. Projected aloft from this crater by a succes- sion of colossal explosions, a vast dome or cone of volcanic smoke on that day covered a region of not less than 400 miles in diameter with absolute dark- ness for many hours, and spread a deep gloom for not less than 1,000 miles in every direction. From the summit of this immense reservoir of vapors piled to an unknown height, the great Equatorial Haze-stream, appears to have issued, and sped westward around the globe. "We have unquestionably traced it to its source in the vapor-mass that overhung the Indian Ocean less poetic than a cosmic nebula, but possessing reality, and with it have found the one sole and indisputable origin of the Bed Glows which attended its course. This does not imply that the swift Equatorial Smoke-stream embodied the whole of the glow-producing medium. It seems more probable that the larger portion of the vapors which became slowly and irregularly diffused over the globe during the ensuing seventy days, were drifted from the broad vapor-mass after the special stream had ceased. Thus we find the Indian peninsula untouched by the narrow stream which must have passed south of the Equator. But li days afterwards, the haze arrived in full force and produced the Green Suns and- Red Glows throughout Ceylon and South- ern India, shortly afterwards appearing in Aden and the Soudan. We also find the Glows at New Ireland, 3,200 miles due east from Krakatoa, in four days after the last explosions. In all these oases the transportation was comparatively slow, and probably due to atmospheric currents. "We need to consider the adequacy of the eruption of Krakatoa to have produced atmospheric effects of such magnitude and extent, not only " belt- ing the globe with flaming skies," as in September, but by November envel- oping the entire sphere in these fiery glares. Can Krakatoa be shown to have probably ejected a quantity of tenuous matter sufBcient for this result ? And can it be believed to have delivered such matter at such a Tieight that in its descent it would form a haze canopy from 30 to 40 miles above the surface ? "We have absolutely and precisely traced the Glows to their source, and so have the right to afBrm that Krakatoa proved its colossal capacity to emit these vapors in such quantity and to such a height, by having actually done so. It is the objector's part to prove that it could not have done so, and did not. But waiving this advantage, we cite a preliminary of&cial Report on the nature and effects of the eruption of Krakatoa, made bv Mr. B. D. M. Verbeek. V'\ He makes an estimate of the quantity of those solid ejeeta of the crater, which were so coarse as to be speedily precipitated. This amounted to 18 cubic kilometers or 4.5 cubic miles, two-thirds of which fell as ashes and pumice within a radius of nine miles. He believes that at least an equal mass was delivered at the highest parts of the column in the form of vapors and impalpable dust. It would be easy to present considerations to show that this finer portion must have vastly exceeded the coarser. (But this might be speculative. We know that four and a half cubic miles of solid matter would overlay the entire atmosphere of the globe with a solid film of one seven-hundredth of an inch iu thickness. This would doubtless be equivalent to many mile^ in thiokuess of such tenuous vapor and dust as have been floating in the upper ether. 'As to the height of the column of ejeeta emitted from Krakatoa at its highest activity, some estimate may be formed from known facts. The fc. Natfwre, vol. 30, pp. 10-14, 69 heaviest throes -were very precisely determined ['] to have occurred at 9:55 and 10:45 a. m. on August 27th. The latter one was immediately followed by a continuous downpour of mud and ashes upon the ship Charles Bal, then 30 miles distant, [ml Seventy miles away, trees were extensively shattered by the weight of wet ashes. [»J Batavia, 100 miles away, was covered three inches deep with white ashes during the hours of total darkness following the greatest eruption. It seems impossible to find room for these facts on any estimate of the height of the eruptive column, as less than one hundred miles. It is true that light ashes might have great lateral diffusion from a column of far less height, but mud and wet ashes must have plunged quite directly downwards, so that a lateral throw of 30 to 70 miles must involve a vertical ascent of not less than one hundred. The height supposed would have driven the eruptive column entirely through the atmosphere and far above it, so as to deliver its contents over the surface of th» atmosphere, to settle slowly down through its upper strata. That the great column did actually thus lift and rend asunder the mighty mass of the atmosphere above the crater is made probable by the unique oscillations of the barometers. A series of atmospheric waves was sped three times around the globe at the rate of 700 miles an hour, [o] The length of each undulation was one million meters, that of the lowest audible sound waves being 24 meters. Twenty miles away from the crater the mercury rapidly oscillated between the 28th and 30th inches. It is thus evident that in the vicinity of Krakatoa the upper layers of the atmosphere were swing- ing up and down through a vertical distance of from ten to twenty miles every 15 minutes. What could have done this less than an explosion driving clear through its entire depth ? As general evidences of the ultra-colossal character of the Krakatoa explo- sion may be adduced the following : 1. The waves driven upon the coasts of Anjer and Merak, 30 miles away, were found to have exceeded 35 meters or 113 feet in height. Ol Over the entire Anjer plain, fifteen miles by five, the inundation had uprooted every tree, and coral blocks of from 20 to 50 tons in weight had been torn from the bed of the sea and borne inland two or three miles. [«] 2. The detonations of the eruption were heard throughout a circle whose radius is 1,800 geographical miles, W equal to one-fifteenth of the surface of the earth. Yet the heaviest could not be heard within a radius of 40 miles from the crater. The sounds must have proceeded from tremendous rend- ings of the air at an immense height, whence the sounds were easily spread to vast distances, while from localities beneath, the massive torrents of descend- ing e.iecta cut off the sounds like a wall. 3. Ashes fell [«! at Singapore, 335 miles ; at Buncalis, 915 miles N. W. ; at Keeling, 1,200 miles S. W. ; on the Australian coast, 1,050 miles E. S. E. ; on the Arabella, 970 miles W. N. "West. The entire area of ash-fall was ofBcially estimated as at least 750,000 kilometers, Ct] or as large as the Southern States east of the Mississippi. The history of the eruption shows that upon the collapse of the mountain, on the morning of the 27th, the eruptions became submarine ; ["I the ocean waters rushed into the burning depths. Under the pressure of many miles of water the lava and the waters commingled and struggled with geyser-like discharges of augmenting violence, until finally there arose a continuous column of white-hot water and lava. Through the wide throat, apparently three miles in diameter, the vast column drove upwards, expanding and i. Nature, 30, 13. m. Nature, 29, 140. n. LeUrwre How, JiiXy, 1886, page 487. Nature, 29, p. 181. P- Natmre, 30, li—Leiswe Htmr, Sept. 1885, p. 636. 3. Leisure Bam-, August, '188B, p. 558. r. Natwre. SO, 10. .. Nature, 30, 18. t. Nature, 30, }.. 13. ^ Nature, 30, p. 18. TO exploding as it flew into steam and pumice, till reaching ome liundred miles or more in height, its mingled solids and liquids had exploded in the vacuum into thinnest ether. The ashy ejeota, as analyzed, were mainly of glass in the form of pumice, together with the solid constituents of sea- water. M This vitreous matter, being comminated by the force of the explosions to dust of ultra-micro- scopic flnensss, formed together with the vaporized sea^water, a vast bulk of extreme tenuity and lightness above the atmosphere. Falling thence upon the upper strata of the atmosphere, and precipitating its coarser dust, its finer portions have continued suspended for more than two years in their ethereal encampment, and there are likely to abide for many years to come. From the beginning the white sun-glow has been very uniform, while the night-glows have been quite irregular, although it is believed they have always been perceptible. In the northern tropics, there has been a marked increase of Ijrilliancy and continuity during each of the two winters. Probably the haze is distributed through the atmosphere in unequal and irregular drifts. John Aitken's demonstrations of the necessity of dust nuclei to the formation of ice spicules in the atmosphere, C'"] indicate that such ice-parti- cles probably play a prominent part in the Glows. Not improbably they would be in larger quantity in the Tropics during the winter, and so the Glows increase at that season. Varying atmospheric conditions would also at all seasons vary the amount of congelation. In conclusion, the writer takes the opportunity to venture the surmise that a thorough study of the Krakatoa Smoke-belt of September, 1883, and of its dynamic conditions, may furnish material aid in elucidating the still mysterious problem of the Belts of the planet Jupiter. V. Na'ure, 30, p. iS. w Nature, 29. r>. 4C3.