88 



NATURE 



\_Nov. 28, 1889 



are very bright, the compound structure, as seen in the spectrum 

 of a spirit-lamp or the base of a candle-flame, maybe looked for. 

 The star falls in species 9 of the subdivision of the group, and 

 is accordingly of about mean condensation. Dark metallic lines 

 will probably be found to make their appearance about this 

 temperature, and the presence or absence of b, D, or other lines 

 should therefore be noted. 



(3) Vogel classes this with stars of the solar type, but is 

 doubtful whether it does not belong to Group II. It is most 

 likely that it is at an intermediate stage — either a late stage 

 of Group II. or an early stage of Group III. There are 

 evidently traces of some of the dark flutings, and it is suggested 

 that the distinguishing numbers of these and the relative in- 

 tensities of the lines should be noted. The observations made 

 by Prof. Lockyer and myself seem to indicate that the bands in 

 the red are the most persistent as the temperature increases. 



(4) According to Gothard this is a star of Group IV., and 

 the usual observations are required. 



(5) This is classed with stars of Group VI. in Duner's cata- 

 logue, but it is stated that the type of spectrum is rather doubtful. 

 Like the star given last week, it may possibly be intermediate 

 between Groups V. and VI., and similar observations are 

 suggested. 



(6) This is a variable star which will be at its maximum on 

 November 30. Gore gives the period as 281 '2 days, and the 

 range as 8 at maximum to < 11 '5 at minimum. The spec- 

 trum is of the Group II. type, and the suggestions made for the 

 observation of R Tauri (see p. 68) apply equally in this case. It 

 may be further suggested that the spectrum be observed for 

 some time after the maximum, special attention being given to 

 the fading out of the carbon fluting in the green (517, a little 

 more refrangible than b) relatively to the other bright spaces. 



(7) Gore gives the period of this variable (maximum on 

 December 4) as 276 days, and the range as 8 "6 to < 13 '5. The 

 spectrum and colour have not yet, so far as I know, been recorded, 

 and midnight observers may therefore take advantage of the 

 approaching maximum. A. Fowler, 



The Total Solar Eclipse of 1886. — The report of the 

 observations of the total solar eclipse of August 29, 1886, made 

 at the Island of Carriacou by the Rev. S. J. Perry, has been 

 published. The two main questions that required spectroscopic 

 observations to answer them were : — (i) Does the absorption, 

 which produces the Fraunhofer lines, take place mainly in a 

 single layer of the solar atmosphere, or in concentric layers? 

 (2) Does carbon exist in the corona? With respect to the first 

 point. Father Perry thinks that the differences in the length 

 of the lines which he observed before totality on the less re- 

 frangible side of b seems somewhat to strengthen the view that 

 the selective absorption takes place in concentric layers. During 

 totality a search was made for the two principal bands of the 

 ca:rbon spectrum. The part of the spectrum observed was from 

 about b to A560, but no trace was seen of the carbon bands. 

 Father Perry, however, suggests that perhaps the intensity of the 

 carbon spectrum may vary m each eclipse, and may have some 

 direct connection with the amount of solar activity. Some 

 sketches of the coronal streamers are appended to this report. 



Mr. H. H. Turner's report of the observations of the same 

 eclipse, made in the Island of Grenada, has also been received. 

 The following is a list of the lines seen and the jorder in which 

 they appeared : — 



h. m. s. 



7 7 45 ... F line appeared, 



7 8 55 ... 4923 appeared ; very short. 



7 II 30 ... 4923 and 4933. Immediately after, many lines 



appeared. 



7 12 o .., Totality, 



7 20 50 ... Only F ; 4923 and 4933 visible at times, 



7 21 45 ... 4923 still suspected, and 4956. 



7 22 28 ... 4956 ; certainly visible. 



7 24 42 ... No line visible. 



It will be seen that to some extent these observations lead to 

 the same conclusion as that arrived at by Father Perry. 



The corona was examined with a view to the detection of 

 currents, but with a negative result, 



Palermo Observatory. — The fourth volume of observations 

 made at Palermo has beea issued by Prof. Ricco, and covers the 

 period 1884-88. The observations of sun-spots during 1885 

 .'•how that the limiting latitude in whith the phenomena occurred 



were -f 25° and - 30°. Two maxima are indicated by the curve 

 of distribution that has been plotted, both extending from about 

 10° to 15° north and south of the equator, but the number of 

 spots that have been observed in the latter hemisphere consider- 

 ably exceeds that observed in the former. The minimum which 

 occurs between these two maxima is in a latitude slightly 

 north of the equator. Generally speaking, faculae appear to 

 have been equally distributed over the sun's surface. The spec- 

 troscopic observations that have been made of solar prominences 

 in different latitudes demonstrate that the reversal of the coronal 

 line 1474K and b was considerably more frequent a little to the 

 south of the equator than in any other latitude, and was con- 

 tained within the limits -f 30° to - 30°, following somewhat the 

 same line of distribution as that of spots. 



Prof. Ricco has included some fine sunset observations made 

 after the eruption at Krakatab, which support the view that, 

 to a great extent, they were due to the suspension of volcanic 

 dust in the atmosphere. A lengthy series of meteorol epical 

 measurements, some observation of Nova Orionis, Nova An- 

 dromedas, and various comets, are also contained in this 

 publication. 



The Variable Star Y Cygni. — The irregularities before 

 observed in the period of this star have been verified by Mr. 

 Chandler's more recent observations {Astronomical yournal. 

 No. 204, October 1889). He finds that the period of the star, 

 which increased by nearly two minutes during 1887 and 1888, is 

 now decreasing at a similarly surprising rate. The reversal 

 appears to have occurred about the middle of 1888, and the 

 average value for the last twelve months has been about 

 id. iih. 567m. Assuming this average value for the period of 

 the star, an ephemeris is subjoined. Only alternate minima are 

 given. 



Minima of Y Cygni. G.M. T. 



1889. 1890. 



d. h. in. d. h. m. 



727 Dec. 2 12 38 ... 747 Jan. i 11 32*0 



729 ,, 5 12 31-4 ... 749 ,, 4 II 25-4 



731 ,, 8 12 24-8 ... 751 ,, 7 II 188 



733 ,, II 12 i8-2 ... 753 ,, ID II 12-2 



735 „ J4 12 II-6 ... 755 ,, 13 II 56 



737 „ 17 12 50 .„ 757 ,, 16 10 59-0 



739 ,, 20 II 584 ... 759 „ 19 10 52-4 



741 ,, 23 II 51-8 ... 761 ,, 22 10 45-8 

 743 „ 26 II 45-2 

 745 .. 29 II 38-6 



Paramatta Observatory. — The Government Astronomer 

 at this Observatory, Mr. H. C. Russell, F.R.S., has collected 

 and arranged in a concise form the history of what has been 

 done in New South Wales for astronomy and meteorology since 

 1778. The paper may be found in the Proceedings of the 

 Australasian Association for the Advancement of Science, 

 Sydney, 1888, p. 45. 



Minor Planet 282. — This planet, discovered by M. Char- 

 lois, January 28, 1889, has received the name of Clorinde. 



A New Variable Star in Hydra. — Mr. Edwin F. Sawyer,, 

 in the Astronomical yournal, No. 204, gives observations de- 

 monstrating the variability of the star 358 (U,A. ) Hydrse, R.A. 

 I3h. 41m. 59s., Decl. -27° 44 "5 (1875 o). An inspection of 

 the observations that had previously been made of the magnitude 

 of this star indicates fluctuations of about one unit, viz. 7m. to 

 8m., and the period would appear to be about one year. The 

 star is quite red. 



Sun-spots in High Southern Latitudes. — The Rev, S. 

 J. Perry read a paper under this title at the meeting of the Royal 

 Astronomical Society on November 8, in which he drew attention 

 to some remarkable instances which have recently occurred of 

 the appearance of sun-spots at a great distance from the equator. 

 These took place on June 5, June 30, October 8, and October 10 

 respectively ; that of June 30 being especially interesting, as the 



