by R. B. Lucas; "A Graphic Method of Showing the Relations between the Temperature of the Dew Point and the Temperature of the Air for any Given Climate,” by C. W. Adams; "Determining Longitude at Sea," by Capt. Shortt; "Our Tasmanian Earth Tremors," by A. B. Biggs; and "The Science of the Unseen," by Archdeacon Hales.

B. Chemistry and Mineralogy.-This section was presided over by W. M. Hamlet, Government Analyst of Tasmania, whose presidential address had to do with "The Progress of Chemistry in Australasia.” The following-named papers were read: "Note on the Electrolysis of Fused Salts of Organic Bases,” “ Occurrence of the New Element Gallium and Indium in a Blende from Peelwood, New South Wales," "Note on the Volatility of Magnesium" and "Lecture Experimental on Gaseous Diffusion," by J. B. Kirkland; "The Analysis of the Cavendish Banana (Musa Cavendishii) in Relation to its Value as a Food," by W. M. Doherty; "On the Use of the Oleorefractometer in Organic Analysis," by W. M. Hamlet: "On Some Mineral Waters of New South Wales," by J. C. Mingaye: "Analysis of Storage-battery Plates," by A. H. Jackson; "The Jarvisfield Mineral Waters of Picton, New South Wales," by A. J. Sachs; "Minerals of East Gippsland." by Donald Clark; "The Rusting of Iron" and "The Occurrence of Magnetite in Certain Minerals," by Archibald Liversidge; "Notes on the Exudations Yielded by Some Australian Species of Pittosporum," by J. H. Maiden; Note on a Natural Bone Ash from Narracoorte," by N. T. M. Wilsmore; and "Note on an Analysis of Water from Lake Corangamite," by A. W. Craig and N. T. M. Wilsmore.

C. Geology and Paleontology. This section was presided over by Prof. T. W. E. David, who holds the chair of Geology in the University of Sydney, New South Wales. His address treated of the "Volcanic Action in Eastern Australia and Tasmania," with special reference to the relation of volcanic activity to oscillations of the earth's crust and to heavy sedimentation. The following-named papers were read: "On Occurrences of Lepidodendron, near Bathurst, New South Wales" and "Remarks on the Theory of Coral Reefs," by W. J. C. Ross; "An Inquiry into Supposed Indications of Catastrophe," by J. C. Corlette; "On the Age of Mammaliferous Deposits in Australia," by Ralph Tate; "Notes on the Application of Photography to Geological Work," by J. H. Harvey; "Notes on the Late Land Slips in the Dandenong Ranges, Victoria," by F. Danvers Power; "On a Sample of Cone in Cone Structure," by A. J. Sachs; "Description of Mount Bischoff and its Workings," by H. W. F. Kayser; "Fossils from the Tertiary Beds around Bairnsdale," by Donald Clark; "Notes on the Permo-Carboniferous Rocks of New South Wales," by T. W. E. David; and "Notes on the Advantages of a Federal School of Mines for Australasia," by F. Provis.

D. Biology. The presiding officer of this section was W. Baldwin-Spencer, who is Professor of Biology at Melbourne University. His address consisted of a discussion on "The Fauna of Tasmania." Subsequent to a “Report of Committee on the Fertilization of the Fig." the following papers were read: "On the Systematic PosiVOL. XXXII.-3 A

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tion of Bithinia Huonensis " and "On the Affinities of the Florulas of Lord Howe and Norfolk Islands," by Ralph Tate; "On the Origin of Struthion's Birds of Australasia,” by F. W. Hutton; "Notes on Some Land Planarians from Tasmania and South Australia" and "Further Observations on the Eggs of Peripatus," by A. Dendy; "The Markings of Fish with Relation to their Hereditary or Phylogenetic Import," by W. Saville Kent; "Zoological Exploration of Timor" and "The Geographical Distribution of Australian Limicolæ," by W. V. Legge; "On a Trematode with Ciliated Integument." by W. A. Haswell; "Queensland Fungus Blights," by F. M. Bailey; "On the Preservation of our Native Plants and Animals," by A. F. Robin; "Preliminary Note on the Vesicula Seminales and the Spermatophores of Callorhyncus Antarcticus,” by Jeffrey Parker: "Notes and Description of a Young Echidna," by Alexander Morton; "On the Habits of Ceratodus, the Lung Fish of Queensland," by W. Baldwin-Spencer; "Review of Queensland Lichens," by J. Shirley; and List of Tasmanian Mosses," by W. A. Weymouth.

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E. Geography. This section was presided over by Commander Crawford Pasco, R. N., who, in his presidential address, discussed the explorations of Australia and referred to the large area of the globe yet to be explored within the Antarctic circle. Subsequently the following-named papers were read: Report of the Antarctic Committee," "Notes on a Magnetic Shoal near Cossack, W. A.," by W. Osborne Moore; "Explorations and Discoveries in British New Guinea since the Proclamation of Sovereignty," by J. P. Thomson; "Icelandic Notes," by J. B. W. Woollnough; "A Draft of the Great South Land," by A. Mault; "The Influence of Spanish and Portuguese Discoveries on the Theory of a Southern Continent." by J. R. McClymont; "Dispatches from the Elder Exploring Expedition," by D. Murray; Volcanic Phenomena in Samoa in 1866," by John Fraser; and "Life and Work of Sir John Franklin," by A. C. Macdonald.

F. Economic and Social Science and Statistics.-The presiding officer of this section was Richard Teece, the actuary of the Australian Mutual Provident Society, Sydney, whose address had to do with a "New Theory of the Relation of Profit and Wages." The following papers were read: "On International Statistical Comparisons," by Robert Giffen; “The Organization of Industry," by Alfred De Lissa; "The Obligations of a Civil Government," by J. W. Cotton; "The Effects of Protection on the Imports of Australia," by A. Sutherland; "The Incidence of Taxation," by N. J. Brown; "Is Capital the Result of Abstinence?" by A. J. Ogilvy; "Disturbance of the Population Estimates by Defective Records," by H. H. Hayter; “The Evolution of Hostility between Capital and Labor," by Mrs. A. Morton; "The Wealth of Australasia," by T. Coghlan; "The Luneral, or a Table for discov ering Week-day Dates," by W. E. Stopford: "A Layman's Criticism of Current Theories of Population," by S. Clemes; "Insanity and Crime," by E. Pariss-Nesbit and "Australian Currencies,' by A. F. Basset Hull.

G. Anthropology.-This section was presided over by Rev. Lorimer Fison, of Queen's College, Melbourne, who discussed the subject of "An

thropology" as his address, advocating its study and commenting on the advantages offered by British New Guinea and its outlying groups of islands for its pursuit. The following papers were then read: "Bibliographical Report"; Story of Tu and Rei " and " Women's Omens," by Rev. Dr. Gill; New Britain and its People," by Rev. B. Danks; Sydney Natives Fifty Years Ago," by Rev. W. B. Clarke; “Samoa and the Loyalty Islands," by Rev. S. Ella: "Notes on the Tannese," by Rev. W. Gray; "The Loyalty Islands," by Rev. S. M. Creagh; "Malekula Custom," by Rev. W. Legatt; "Aneityum Custom," by Rev. J. Lawrie: "Group Marriage and Relationship" and The_Nair Polyandry and the Diere Piraruru," by Rev. L. Fison; The New Hebrides," by Rev. D. Macdonald; and "The Origin of the Sense of Duty," by A. Sutherland.

H. Sanitary Science and Hygiene. The presiding officer of this section was Prof. W. H. Warren, who holds the chair of Engineering in the University of Sydney. His address dealt with the development of sanitary science and its application to present experiences both in cities and towns and in dwellings. The following papers were read: "Cremation," by T. James; House Ventilation," by P. Hurst Seager; "The Etiology of Typhoid," by E. O. Giblin; "Physical Education in Schools," by Miss Violet Mackenzie: Notes on a Grease Interceptor," by W. S. Cook; "Sewerage of a Seaside City," by A. Mault; "On Some Matters relating to Public Health," by C. E. Barnard; Diseases communicable from Animals to Man, illustrated by Microscopic Slides," by A. Park; and “On the Modes of Infection in Tuberculosis," by E. Hirschfeld.

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I. Literature and Fine Arts.-Prof. Edward E. Morris, who has the chair of English, French, and German Languages and Literatures in the University of Melbourne, was the president of this section. His address had to do with education, and he advocated fewer universities but increased teaching facilities. The following papers were read: The Heralds of Australian Literature," by T. A. Browne; "Some Aspects of Australian Literature," by Alexander Sutherland; Among the Western Highlands of Tasmania," by W. Č. Piguenit; "Popular Errors about Art and Artists," by J. R. Ashton; "The Province of the Amateur in Art," by C. H. Dicker: "The Authorship of Shakespeare's Plays," by F. J. Young; 'Shakespeare and Bacon," by C. M. Tenison; 'Secondary Education in Australia," by P. A. Robin; Elementary Science in Primary Schools," by J. Rule; "The Scientific Method of studying Languages," by R. T. Elliott: "The Rationale of Examinations," by F. J. Young; "The Modern Lyric from a Musical Standpoint," by Miss E. Mills: "Tennyson's Poetic Rhythms," by H. R. Webb; "The Australian Decorative Arts," by J. R. Tranthim-Fryer; and Formation of Home Reading Union," by the Bishop of Tasmania.

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J. Architecture and Engineering. This section was presided over by C. Napier Bell, of Greymouth, New Zealand. His address was general, and described the more prominent of the recent developments in engineering science with their special suggestiveness to Australia. Papers

with the following titles were read: “Building and Architecture; a Definition and a Vindicator," by Alan C. Walker; "The Truthful Treatment of Brickwork," by A. North; On the Making of Hydraulic Lime and Mortar," by A. O. Sachse; Primitive Construction of Houses," by Edward Dobson: "Railway Extension and Break of Gauge," by A. Stuart; "Water Supply of Rural Towns of Tasmania," by C. W. James; "City Surveys," by D. M. Maitland; and Fronts of Buildings in Brickwork v. Portland Cement," by W. W. Eldridge.

Entertainments.-During the meeting the following evening lectures were delivered: On Jan. 8. "The Rise and Growth of the British Empire," by Dr. Robert Giffen; on Jan. 11, “The Great Sutherland Waterfall," by C. W. Adams; and on Jan. 13, “Early Hobart," by J. B. Walker. On Jan. 12, a concert was given by the Musical Union; also garden parties were given, on Jan 7, by Sir Robert G. C. Hamilton; on Jan. 9, by Henry Dobson; on Jan. 13, by the Bishop of Tasmania; and on Jan. 15, by R. C. Read. On Sunday, Jan. 16, a science sermon, "From Man to Nature and from Man to God," was delivered by Rev. George Clarke, Vice-Chancellor of the Tasmanian University.

Next Meeting.-The fifth annual meeting of the association will be held in Adelaide, South Australia, in 1893, at a time which was left to be fixed by the officers and committee in Adelaide. For that occasion the following officers were chosen: President, Prof. Ralph Tate; VicePresidents, Sir Robert G. C. Ilamilton, Baron Ferdinand Von Mueller, Sir James Hector, Albert Norton, and H. C. Russell; General Secretaries, E. H. Rennie and W. H. Bragg; and Local Treasurer, F. Wright.

ASTRONOMY, PROGRESS OF, IN 1892. The astronomical discoveries of the past year have been numerous and important, as the following résumé will show:

ics.

The Sun. Although the present is only the second or third year of the sun-spot maximum cycle, yet the number and enormous dimensions of some of the groups and isolated spots, often visible to the naked eye, have excited much popular as well scientific interest in solar physAstronomers were greatly surprised at the immense size of a sun spot which appeared in September, 1891, though it was but a pygmy in extent when compared with that of February, 1892. The latter was for several days conspicuously visible to the naked eye. To record its history from its inception to its final disappearance after five axial rotations of the sun would occupy more space than this limited article will allow. Though called a sun spot, it was, in reality, an aggregation of fifty or more separate but contiguous spots, which seemed to have been thrown out from the center in wild profusion as if by an explosion. At its maximum, on Feb. 8. it is doubtful if there ever has been seen so grand a spectacle on the sun's face. As 450 miles at the sun's distance subtends an angle of but 1", and as the spot was 5′ 30′′ = 148,500 miles in length, and 3' 15" 87.750 miles in breadth, it follows that it must have covered an area equal, in round numbers, to 10,000,000,000 square miles, concealing of the sun's visible hemisphere. During its visibility it drifted in lati

tude from 17° S. to 30° S. It was not seen at the sixth rotation of the sun upon its axis.

The diminution of light by an obscuration so extensive would equal the loss of 5,000 full moons. Whether this, when seen from a star,

THE SUN-SPOT OF FEBRUARY, 1892. Feb. 5, 10.35 A. M.

would be sufficiently noticeable to rank our sun as a variable star, as many suppose, is exceedingly doubtful. No diminution of either the sun's heat or light upon the earth is shown by delicate tests when the orb is so largely covered, but remains the same in these particulars as when it is spotless.

Solar Prominences.-Solar activity has not been less marked in regard to the prominences than in sun spots. M. Trouvelot, of Janssen's Observatory, at Meudon, France, makes a report of those observed during March, April, and May. He says that out of 40 observed, 23 belong to the eruptive type. April was especially rich in extraordinary outbursts. The base of one seen on April 6 extended 12° along the solar circumference, and had a length of 90,050 miles, and a height of 57,570 miles. On the 8th, one, appearing like a candle flame in shape, rose to a height of 71,970 miles at 10h 54m, and a half-hour later had attained a height of 105,550 miles.

visibly connected with the outburst, and a sun spot near was undisturbed. The observer adds. that a velocity so great carried the matter into space beyond the sun's attraction, and so, of course, beyond return. May not such eruptions of matter be the source of the sun's corona, and the zodiacal light and of the Gegenshein?

Sun Spots and Terrestrial Magnetism.-It is rather generally conceded, though disputed by some eminent authorities, that during the prevalence of sun spots the earth's magnetism is intensified, and auroral phenomena are more numerous. The number of auroras and magnetic disturbances, both of the earth and its atmosphere during the present year, especially on the apparition of the great sun spot of February last, seem to be proof of its truth. Numerous instances through many years may be cited confirmatory of the relationship. On the other hand, it is noteworthy that auroral and terrestrial magnetic disturbances often occur during solar quiescence, but the Astronomer Royal, Mr. Christie, argues that, seeing but one side of the sun at such a time, there may have been a spot on the other side. He further says: There are now three or four marked cases on record of large spots on the sun being coincident with these disturbances on the scale experienced last February, but there are no cases of a large spot being seen without magnetic disturbances."

Solar Spectrum.-Lines in the invisible ultraviolet portion of the solar spectrum have, for the first time, been photographed by H. Deslandres using a Foucault siderostat with an eight-inch Rowland grating. The lines due to hydrogen in this part of the spectrum, first observed by Huggins, have also been photographed in the spectra of the protuberances, eight of the ten belonging to the series having been seen. It is believed that from a mountain elevation the other two could be detected. Photographs of the spectra

minutes rose to a height of 140,000 miles, having ascended at the rate of 228 miles per second. Later, the lower portion faded, but the upper part continued to rise until an elevation of 237,000 miles was reached. No spot or facula was

of faculæ and sun spots show the H and K lines of calcium more intense than those of hydrogen.

Spectroheliographic observations of the sun have been made by Prof. George E. Hale, of Kenwood Observatory, Chicago. In a paper

read before the meeting of the American Association for the Advancement of Science, at Rochester, in August, he described the ingenious apparatus which he had invented and perfected for photographing the spots, the faculæ, and the prominences. This device records faculæ which the eye can not detect. He secures on one plate, with one exposure, the spots, faculæ, chromosphere, and the protuberances, and exhibited before the association, by the aid of the optical lantern, the first complete picture of the sun ever taken. The reader will find a description of the spectroheliograph in Astronomy and Astro-physics" (late" Sidereal Messenger") for May, 1892, published at Northfield, Minn.

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Prof. Hale's achievement in photographing ten bright lines heretofore unknown in the ultraviolet spectrum of the prominences and the chromosphere is an unrivaled one, and excites great interest among astronomers and spectroscopists. By the aid of a new objective by Brashear, which by its color correction is well adapted to this kind of work, he has photographed nineteen lines in the ultra-violet.

A photograph of importance was taken on July 15, showing simply a large spot. A few minutes later another was secured in which a bright band had developed. Twenty-seven minutes after the last named, another plate showed bright faculæ covering nearly the entire spot, which, however, soon disappeared, and the spot at the final exposure presented the same appearance as on the first plate. The accurate photographic delineation of such sudden changes is justly regarded as greatly important. On the day following these observations, a magnetic disturbance and brilliant aurora were noted. Prof. Hale estimated the size of the spot to have been 4,000,000,000 square miles.

The Sun's Diameter.-In Astronomische Nachrichten, No. 3,066, Dr. Auwers gives the results for solar parallax from the German transit-ofVenus expeditions in 1874 and 1882. That of the transit of 1874 is 8.877" ± 0·043, and that of 1882 equals 8-879" ± 0·037.

In the same journal, No. 3,068, the same writer has a paper on the diameter of the sun as determined by the heliometric measures made in connection with the above-named expeditions by 31 observers with 4 instruments. He finds the mean results for the sun's mean diameter to be 1,919.3", which differs considerably from that at present adopted by the various nautical almanacs, the German being 1,922-4", the French and English 1,923-6", and the American 1,924-0". Dr. Auwers remarks that, if the value he finds is influenced by irradiation effects, it can only be too large, and thus the errors of the adopted diameters must be greater still. He urges that an immediate change in these values be made, and announces for the "German Almanac " that the alteration will occur in the volume for 1895.

The observations are discussed for possible ellipticity of the sun's disk, with the result that the polar diameter is found to exceed the equatorial by 0-032. Had the personalities of the observers, in both perpendicular and horizontal observations, been taken into consideration, the value for the polar diameter, it is believed, would have been less, as indeed it ought to be, considering the sun as a rotating body. But an ellip

ticity of so small an amount as± 0.038" is immeasurable, and indicates that a deviation from an exact sphere has not been and can not be proved.

The Cause of Solar Heat.-In the recently issued volume of "Transactions of the Astronomical and Physical Society of Toronto," Dr. Joseph Morrison, of the American Nautical Almanac" office, has a paper treating of the two most generally received theories of the source and maintenance of the enormous heat of the sun. One hypothesis is that it is due to the energy developed by the falling of meteoric matter on the sun. The other asserts that it is produced and kept up by slow contraction of the sun's bulk. He calculates that a pound of matter falling from infinity would develop 82,340,000 units of heat, and, therefore, that a quantity of matter equaling one one hundredth of the earth's mass falling annually on the sun would maintain an amount of heat equal to that observed.

As to the contraction theory, he says, taking the solar constant at 25 calories per square metre per minute, the linear contraction of the sun's radius requisite to keep up the present radiation is 1569 feet in a year, or nearly 30 miles in a thousand years. As 450 miles of the sun's diameter subtends, at the earth's distance, an angle of only one second of arc, it would, therefore, require 7,575 years for the sun's angular diameter to be reduced by one second of arc, the smallest angle measurable on the sun's disk.

Direction of the Sun's Motion.—A little more than a hundred years ago Sir William Herschel, noticing that the stars in the constellation Hercules were slightly farther apart, and that those in the opposite direction were nearer together than as determined prior to his day, came to the conclusion, and so announced, that our sun, with the entire solar system, had a progressive mo tion in the direction of Hercules. This theory has never, from subsequent observation, been disputed, save as to the exact direction of its motion.

Prof. Lewis Boss, Director of the Dudley Observatory, has exhausted the refinements of mathematical and observational astronomy only to establish its truth. He, however, places, as the result of his calculations, the "apex of the sun's way" in R. A. 289°; Dec. + 51°, or in Cygnus instead of Hercules.

McStumpe has likewise made thorough investigation of the complex problem, but his results differ somewhat from those of Prof. Boss. His mean of four determinations gives R. A. 285°; Dec. north 36°, or between Cygnus and Hercules.

The Moon.-Lunar Radiant Heat.-The second series of Vol. IV of the Scientific Transactions of Royal Dublin Society contains a memoir on the moon's radiant heat as determined by Dr. Boeddicker at the observatory of Lord Rosse, Birr Castle, Ireland, during the total lunar eclipse of Jan. 28, 1888. His conclusion was that the moon's heat has much lower refrangibility than the sun's, and that the maximum of heat falls rather before than after the time of full. The results of this eclipse fully confirmed those of that of 1884, the radiation falling considerably below the commencement of the eclipse and not returning to its standard value until 1h 40m after last contact with the penumbra. He considers the fact es

tablished that the decrease of heat had begun quite three minutes before first contact with the penumbra, a conclusion implying that the earth's atmosphere is capable of exercising a distinct heat absorption at a height of 190 miles. Prof. Frank W. Very, of the Allegheny Observatory, sought the solution of this problem in a different manner, and, instead of choosing an eclipse, observed the moon in different phases, using a bolometer in conjunction with a siderostat for that purpose. The apparatus was so constructed as to enable him to view the entire moon or but a portion of it. He adopted the latter method, and, the lunar image having been projected on a white card in which a small hole had been pierced, the image of the region whose heat was to be measured was brought over this hole through which the rays passed to the sensitive surface of the bolometer. The results thus obtained are given in a series of eight charts on which are marked the different spots whose heat had been observed; corresponding tables give the measures, and isothermal lines inferred from these measures are drawn on these charts. On the portion of the moon to which the sun is setting the heat gradient was found to be more steep than on that part to which the sun is rising. The following are the main conclusions:

1. The existence of a small heat-storing action by which an excess of heat (not more than 10 per cent.) is accumulated after many days of isolation seems to be established.

2. The circumferential zone of the full moon radiates about 20 per cent. less than its center. 3. Bright regions radiate only a little more than the dark, though they reflect nearly twice as much.

4. There is a somewhat larger proportion of reflected rays from the full moon than from the moon at first quarter.

5. The result obtained by Dr. Boeddicker as to the different law followed by the diminution of heat from that followed by the decrease of light during an eclipse, seems to be confirmed.

Prof. Very, for his paper, was awarded the prize offered by the Utrecht Society of Arts and

Sciences.

Active Lunar Volcanoes.-In the June number of Observatory." 1892, Prof. William H. Pickering has an interesting article from Arequipa, Peru, March 28, 1892, entitled "Are there at Present Active Volcanoes on the Moon?" After describing the atmospheric conditions at the observatory some 8,000 feet above tide, where a magnifying power of from 800 to 1,200 may be used to advantage, he discusses the question of active volcanoes on the moon. Comparing his own observations with the chart of the moon published by Neisen, he says: "Of a total of 67 craters, 32 were found common to both charts, 24 were given by Neisen and not found by myself, while 11 were found that were not given by Neisen. Using the 13-inch Clark telescope, all of Neisen's craters were found save two, which could not be found with a power of 800. The 11 other craters found by myself were all confirmed and a great number of other smaller ones were also seen."

A committee's report to the British Association, some twenty years ago, on the conspicuous crater Plato, mentions 36 luminous points or crater cones, No. 4 of which has entirely disappeared, only a whitish stain at present occupying its place. Nos. 7 and 31 are also missing,

but eight miles southeast is a large crater not reported by the committee. In class three as to size, out of the six recorded only one (No. 16) is now visible. These facts, taken in consideration with the falling in of the walls and the filling up of the well-known crater Linné, may well suggest the question heading this paragraph.

It may be added that No. 4, alluded to above, was seen as a conspicuous crater in 1880, 1882, 1887, and 1888.

Comets. Since Oct. 2, 1891, the date of the latest discovery of a comet given in our last volume, the following comets have been discovered, named in the order of their finding rather than their perihelion passages:

Comet a (Swift) was discovered by Dr. Lewis Swift, at the Warner Observatory, in the early morning of March 6, in the constellation Sagittarius. Though detected with a telescope, it was visible (knowing its place) to the naked eye. It is still (Oct. 14) visible telescopically, and has proved a most remarkable body. As photographed on March 10 by Prof. II. C. Russell at the Sydney Observatory, Australia, it showed eight tails, two of which extended beyond the plate. On the sides of these two long rays three new streamers appear. All of these rays or actinic tails are easily seen on the photographic plates, though none were visible to the eye with the 114-inch telescope.

Prof. Barnard's photographs of the comet, made at the Lick Observatory with an hour's exposure, reveal, spreading out from the head, a complicated system of a dozen tails, some of

which show remarkable curvatures. In less than twenty-four hours the third tail had formed to the extent of 10,000,000 miles, while the northern one had entirely disappeared. His camera was made to follow the comet, so that the stars in the field are represented by lines instead of dots. A picture secured on April 8 shows interesting changes in the tails, a large protuberant mass or semi-tail being seen on the southern side of the principal branch, which developed into a number of thin wisps not before noticed. On one occasion the tail was twenty degrees long, as seen by the naked eye. The following elliptic elements have been computed for it by Dr. A. Berberich, of Berlin:

Time of perihelion passage, 1892, April 6-69025, Berlin mean time: From node to perihelion = 24° 81' 11-1" Longitude of node =240° 54' 15:4" Inclination = 85° 42′ 20 6" =1·02606 = 0.998611

Ferihetion distance Eccentricity

While its eccentricity is indicative that it is a periodic, yet its so near approach to a parabola must give it a period of several thousand years. Much uncertainty exists regarding the periodicity of a comet whose eccentricity is so nearly equal to 1.

Comet b (Denning) was discovered by W. F. Denning, at Bristol, England, in the constellation Cepheus, on March 18, 1892. It was excessively faint, and has so remained. The following parabolic elements have been calculated by Dr. Berberich:

Perihelion passage, 1992, May 11-22042, Berlin mean time:
Node to perihelion =129° 18' 34.4"
Longitude of node = 253° 25′ 41-6"
Inclination
= 89° 42' 4-3"

Perihelion distance = 1.97064