35 3963 36

des rCsultats acceptables, il convient d'essayer aussi les multiples et sous-multiples de ce nombre.

Enfin Hartmann a reconnu le fait nouveau suivant: la raie du calcium R 393, qui est fine dans I'Ctoile, n'offre

pas de deplacement variable, et la vapeur correspondante a une vitesse radiale constante. J'ai chercher verifier ce fait tr&s curieux sur mes Cpreuves ; malheureusement, Yin- tensite du spectre dans la region, n'etait pas assez forte.

H. Deslandres. __ Meudon, le 10 juillet 1904.

Seventy - six new variable stars. ( H a r v a r d C o l l e g e O b s e r v a t o r y Ci rcu lar No. 79).

Since the publication of Circular No. 78 (A. N. 3950), in which was given a list of 7 1 variable stars in the Great Nebula of Orion, a further examination of the region has been made by Miss Lcavitt. The plates mentioned in the former circular were superposed successively upon a glass positive made from one of them. In this way, all the vari- ables which show striking changes and are comparatively bright were rediscovered, and nine new ones were found. Six of them are outside of Bond's map, which was the region covered in the previous investigation. Additional plates have been examined for those of Wolf's variables which were not confirmed, with the result that 48 .1903 has been found to be certainly variable. On Oct. 26, 1897, its magnitude was 14.8, and on March 3, 1904, it was 13.7. No variation was found in the star north of it, 54.1903. The star 8 . 1904 does not show variation on the Harvard photographs, being always fainter than the fifteenth magni- tude. Marked variation, however, has been found in I I . I 904, whose magnitude was 14.9 on Jan. 8, 1894, and I 1 .4 on Jan. 22, 1897.

An examination has been made of the stars near the Trapezium, which have been suspected of variability by Bond and other observers, especially Nos. 575, 589, 622, 641, 647, 654, 671, and 676 in Bond's Catalogue. On a few plates having short exposures, these stars can be seen, and show apparent fluctuations in brightness. I t is probable that photographs taken with a telescope of great focal length, would settle this question.

The positions given by Wolf, of the variables dis- covered by him, agree very closely with those found from the measures of Bond. In four cases, Nos. 2 5 , 26, 35, and

T a b l e I. Var iab le s t a r s i n O r i o n a n d Carina.")

, I I I I

114 '904 115 .1904 1 1 6 . 1 9 0 4 1 1 7 . 1 9 0 4 1 1 8 . 1 9 0 4 1 1 9 . 1 9 0 4 1 2 0 . 1 9 0 4 1 2 1 . 1 9 0 4 122 .1904

sh2qrn Is 5 2 5 I3 5 21 5 5 2 7 8 5 30 25

5 30 33 5 3 2 2 2

5 33 32 5 33 34

53, in Table I of Circular No. 78 (A. N. 3950), the positions differ by an appreciable amount. Plates taken on Jan. 25, 1894, and on Dec. 3, 1901, were superposed and examined carefully, but no evidence was found of proper motion during the interval. The right ascension of No. 5, given as 5h 2trn54io in Table II, should read 5 h 2 7 m 4 5 ? 0 .

A cursory examination of the vicinity of 7 Carinae has been made on six plates by the method described above. Ten new variables were found, besides the known variable, U Carinae. None of these are in the nebula. A similar examination of the Small Magellanic Cloud resulted in the discovery of 5 7 new variables, including three in the cluster 47 Tucanae, which appears on the same plates. These variables may be only a small portion of those actually existing in this region, as nearly all of them were found in a comparison of two plates. The known variable, ... Tucanae, oh 54Yz - 75" 32', in the Provisional Catalogue, Annals, XLVIII, No. 3, and six of the eight known, variables in the cluster 47 Tucanae, were also found. A provisional scale of magnitudes has been adopted, as absolute magnitudes of the faint stars have not yet been determined.

A careful examination has been made of the Trifid Nebula. In the region 30' square, whose limits in 1900 ex- tend from right ascension 1 7 ~ 55912 to 1 7 ~ 57414, and from declination - 2 2 O 47' to - 23O I 7', I 167 star images have been examined on two plates and no variabIe found. A similar examination of NGC. 2070, the Looped Nebula in the Large Magellanic Cloud, covered the region whose limits in 1900 extend from right ascension 5h37m6 to 5 h 4 ~ m 2 , and from declination -69Oo' to -69O20'. Out of 867 star images examined, two are suspected of slight variability.

- 6" I 1:3 - 4 33.9 - 5 0.1 - 2 53.7 -5 24.8 -6 51 .7 -6 38.6 - 2 48.0 - 2 47.5

I 1.6 I 2.4

9.0 11 .4 12.8

8.0 11.6 I 1.4

10.0

< I 5 . 4 13.1

I 1 .4 1 2 . 5

'3.5

1 3 . 2 14.2

11.0

1 0 . 2

I 0

I 1 I 2

' 3 ' 4 I 5 1 6 1 7 18 I9

123 . I904 124 . I904 1 2 5 '904

1 2 7 . 1 9 0 4

1 2 9 . 1 9 0 4

126 I904

128. I904

130. I904 131 . I904 132 . I904

I oh I 6418 10 20.9 10 34.6

10 36.4

1 0 49.9 10 50.2 10 50.4 10 5 1 . 3

1 0 34.1

I 0 47.0

-60'57' -60 24 -58 41 -60 1 6 - 5 1 25 -59 49 -51 59 - 5 1 5 2

-60 24 -'58 1 5

1 0 . 0

1 0 . 2

I 1.4 '3.4

13.1 12.6 13.1 '3.4 9.2

11.1

11 .5

13.0 < 1 5 . 1

12 .8

<15.1 '4.9

< 1 5 . 1

14.5

1 2 . 2

1 0 . 2

") Die provisorische Numerierung I 14-122.1904 Orionis, resp. 123-132. I904 Carinae ist von mir hinzugefugt worden. Kr.

37 3963

2. This is the following of two stars which are usually

5 . This star is Bond 663. 6. This star is Bond 726. 7. This star is -701132, and Bond 1036.

8, 9. Apparently these two adjacent stars vary alter-

of about the same magnitude. nately. On the plates examined, one is always bright when the other is faint.

10, I I . These stars are near the edge of the plates examined, and estimates of their brightness were made with difficulty.

19. This star is C.P.D. -6002386. Variability dis- covered by Professor E. c. Pickering.

The new variables in Orion and Carina are given in Table I. A number for reference, the designation, the position for 1900, and the brightest and faintest magnitudes observed on the plates, are given in the successive columns.

In Table 11, the new variables in the Small Magellanic Cloud are given in a similar form as Table I.

T a b l e 11. V a r i a b l e s t a r s i n t h e r e g i o n o f t h e S m a l l M a g e l l a n i c Cloud.*) - No. __

I

2

3 4 5 6 I 8 9

I 0 I 1

I 2

I 3 I 4 I 5 16 ' 7 I 8 I 9 2 0

2 1

2 2

23 24 2 5 26 2 1 28 29

a 1900

oh 9"5 o 18.9 0 2 0 . 2

0 2 0 . 2

0 2 0 . 7

0 24.4

0 34.1 0 35.4 0 36.1 0 31.' 0 37.5 o 38.0 0 38.3 o 40.1 0 43.3 0 44.8 0 45.6 0 45.9 0 46.4 o 46.8

0 33.6

0 41.2 0 41.7 0 41.8 0 49.3 0 50.3 0 50.1 0 52.4 0 52.4

d 1900

- 73" I I'

- 1 2 40 - 7 2 2 1

- 1 2 38 - 1 2 36 - 1 2 44 -14 31 -14 30 - 1 2 34 -14 I 4 -14 16 -11 I 0

-74 11 -74 5 -74 10

-73 16 -73 0

-73 5 5 -13 3 -13 46 -13 18 -74 6 -14 8 -73 11

- 7 0 2 5 - 1 2 49 -73 10

- 1 2 5 - 7 2 31

____

- Br .

11.8 I 1.4 I 1.5 I 1.7 I 1.4 I 1.9 13.9 13.8

13.0

13.6 10.8 13.0

1 2 . 0

1 2 . 0

1 2 . 1

11.1

12.6 13.6 1 2 . 7

13.6

14.2 14.4 12.3

9.4

13.2 'I 2.8 11.7

11.1

11.1

- Ft.

13.4 '3.3 I 2.4 I 2.3

I 2.4 12.6 14.7 '4.7 13.2 14.4 13.1 14.4

13.8 '3.3

'3.7 '4.3 '3.9 15.0

I 5.0 I 5.0 13.6 14.3

'3.9 '3.1 I 2.8

12.1

1 2 . 0

1 2 . 1

1 2 . 0

- No.

30 31 32 33 34 35 36 31 38 39 40 41 42 43 44 45 46 41 48 49 50 5 1 52 53 54 55 56 5 1

~

a 1900

oh5 2914 0 53.6 0 54.5 0 54.9 0 55.0 0 55.1 0 55.4 0 56.4 0 56.5 0 51.7 0 57-8 0 58.4 0 59.4 I 0.7

I 2 .5 I 2.7

I 3.8 1 4.4 I 4.8 I 5.0 I 5.8 I 7.5 1 1.9 I 10.4 I 10.8 I 26.1 I 32.0 I 38.9

~~

6 1900

- 13" 44' - 7 1 48 - 7 2 51 - 1 2 19 - 1 2 58 - 1 2 59 - 7 2 2 1

-13 2 5 -13 59 - 1 2 44 - 1 2 42 -10 34 - 7 2 31 -73 I - 7 2 56 -74 11

-73 48 -73 45 - 7 2 3 -74 16 - 7 2 35 -73 8 - 7 7 23 -13 3 -72 I 3 -74 18 - 7 5 43 -75 1

Br.

13.6 13.4 12 .5

14.0 13.8 12.9 14.0 13.1 13.9 I 1 . 8 14.5 10.8 '3.1 13.4 13.1 13.4 I f . 9

I 2.9 I 2.9 13.4 13.3

13.4 12.9

1 2 . 0

11.0

1 1 . 2

11.0 I 1.6

Ft.

14.9 14.3 13.2 '4.9 15.0 14.5 '4.9 14.0 14.6 13.4 I 5.0

1 5 . 2

14.9 14.5 14.2 13.2 12.9 13.7 '3.5 14.7 14.3 13.4 14.3 14.1

: 14.5

12.0

12.5 12.5

Probably, Nos. 11, 13, and 25, are variable stars of long period, while Nos. 9, 10, 18, 20, 28, 31, 33, 34,

Harvard College Observatory, 1904 May 26. Bawara C. Pic4erin.y. 36, 44, 46, 48, and 53 have periods that are short.

*) Da die Sterne durch die Zugehorigkeit zur kleinen magell. Wolke und die Pickeringsche Numerierung geniigend gekennzeichnet Nr. 1-51 , 53 und 54 liegen im Sternbilde Tucana, 52 und sind, kann von einer besonderen provisorischen Numerierung abgesehen werden.

55-57 im Sternbilde Hydrus. Kr.

Beobachtung von W Ursae majoris. Neben drei Maxima am 10. Januar 1904, 7h 5om, 2 7 . Januar, IO* und 7. Februar, 8h 3grn (unsicher), habe ich

folgende Minima beobachtet: Jan. 1 0 9h 50"; Jan. 1 7 9h 59"; Jan. 2 7 6h 1 7 " (unsicher) und loh 1 2 ~ (gut); Febr. 1 7

1 0 ~ 4 0 ~ ; Febr. 19 6h43m; Mar, 14 7 h 3 ~ m , aber die drei letzten Beobachtungen weniger sicher, die letzte etwas zu spat. Zreitangaben in M. E. Z.

Landstuhl, 1904 April 17. Ph. F a d . 3"