Peremennye Zvezdy

Article in PDF
"Peremennye Zvezdy",
Prilozhenie
,
vol. 8, N 24 (2008)

A Study of Seventeen Variable Stars

E. V. Kazarovets, E. N. Pastukhova
Institute of Astronomy, Russian Academy of Sciences, Moscow, Russia

ISSN 2221–0474

Received:   7.06.2008;   accepted:   23.06.2008
(E-mail for contact: helene@inasan.ru, pastukhova@sai.msu.ru)


#NameOtherCoord (J2000)TypeMaxMinSystemPeriodEpoch (JD)typeSpCommentL.CurveFind.ChartData
1 GSC 0802-0123208 11 16.00, +11 56 57.8RV11.211.5V66.2554467.7min Comm. 1081116lc.jpg081116ch.jpgASAS 081116+1157.0
2 ASAS 091605-2339.309 16 05.45, -23 39 19.6M12.7<15.0V22853446max Comm. 2091605lc.jpg091605ch.jpgASAS 091605-2339.3
3 NSV 06438IRAS 13441-664113 47 50.10, -66 56 43.3M13.4<15.2V388:54560maxM9Comm. 3NSV6438lc.jpgNSV6438ch.jpgASAS 134750-6656.7
4 NSV 06446GSC 7266-0163713 47 52.56, -31 04 01.3RRAB13.614.8:V0.48877453898.5827max Comm. 4NSV6446lc.jpgNSV6446ch.jpgASAS 134753-3104.0
5 NSV 06447IRAS 13450-664513 48 47.71, -67 00 04.8M12.5<16.0V29053831maxM8 NSV6447lc.jpgNSV6447ch.JPGASAS 134848-6700.1
6 NSV 06448IRAS 13453-715613 49 27.43, -72 11 40.7M12.5<15.0V35353562max  NSV6448lc.jpgNSV6448ch.jpgASAS 134927-7211.7
7 NSV 06492GSC 7802-0102013 55 41.80, -44 38 56.9EA7.808.07V1.1655354302.6004minA2Comm. 7NSV6492lc.jpgNSV6492ch.jpgASAS 135542-4438.9
8 NSV 06501GSC 3033-0029813 55 51.99, +44 31 17.3RRAB13.514.6R0.5483651361.7519max Comm. 8NSV6501lc.jpgNSV6501ch.jpgNSVS 5092607
9 NSV 06495HV 855213 56 59.48, -70 35 17.0M12.6<15.0V17154565max  NSV6495lc.jpgNSV6495ch.jpgASAS 135659-7035.3
10 NSV 06507IRAS 13549-560613 58 17.12, -56 21 11.3SRB7.37.8V314 maxC NSV6507lc.jpgNSV6507ch.jpgASAS 135817-5621.2
11 NSV 06532HV 855714 06 00.10, -68 44 12.2M13.5<14.4V28453464max Comm. 11NSV6532lc.jpgNSV6532ch.jpgASAS 140600-6844.2
12 NSV 06577HV 856914 13 55.87, -76 13 05.9M14.1:17.0:R22451915max Comm. 12NSV6577lc.jpgNSV6577ch.jpgASAS 141356-7613.1
13 V541 Oph 17 37 35.38, -23 49 04.9RV13.114.7V58.952545.5min Comm. 13V541lc.jpgV541ch.jpgASAS 173735-2349.1
14 GSC 7909-0168218 28 28.62, -42 51 25.1M12.0:<15.6R22754298max Comm. 14182828lc.jpg182828ch.jpgASAS 182829-4251.4
15 ASAS 184840-3933.318 48 40.12, -39 33 19.4SRA12.314.4V135.754365max Comm. 15184840lc.jpg184840ch.jpgASAS 184840-3933.3
16 IRAS 19000-141919 02 55.81, -14 15 01.8SRA11.7<12.9V21353642max Comm. 16190255lc.jpg190255ch.jpgASAS 190256-1415.0
17 IZ Del 20 36 38.38, +17 57 16.0SRA12.214.0V106.553643max Comm. 17IZDELlc.jpgIZDELch.jpgASAS 203638+1757.3

Comments:


1. Classified as an EC/CW star in the ASAS-3 catalogue.

2. The variability was discovered by Chen et al. (2006) who classified the star as a Mira with P = 200d.

3. The ASAS-3 range is for the combined brightness of the Mira and its neighbor.

4. M-m = 0.13.

7. MinI = MinII. D = 0.21.

8. M-m = 0.15.

11. The brightness limits from Luyten (1933b) are 15.4 - 18.2 pg.

12. The ASAS-3 range is for the combined brightness of the Mira and its neighbor. The limits, given in the Table, are our eye estimates of the star's brightness on the red images from the USNO Image and Catalogue Archive.

13. Classified as a CWA star in the ASAS-3 catalogue.

14. The ASAS-3 range is for the combined brightness of the Mira and its neighbor; classified as a CW star in the ASAS-3 catalogue.

15. Classified as a CW star in the ASAS-3 catalogue.

16. Classified as a CW star in the ASAS-3 catalogue. The ASAS-3 range is for the combined brightness of the SRA and its neighbor. Possibly a Mira variable.

17. Classified as a MISC star in the ASAS-3 catalogue and as a possible CW star with a period about 11 days in Richter (1970). J - K = 1.1 (2MASS).

Remarks:
We could study the variables thanks to the publicly available electronic archives of CCD observations of the ASAS-3 (Pojmanski, 2002), ROTSE-I/NSVS (Wozniak et al., 2004) surveys and the US Naval Observatory Image and Catalogue Archive (http://www.nofs.navy.mil/data/FchPix/). We recovered the variables NSV6438, NSV6447 and NSV6495 suspected by Luyten (1934), NSV6448 and NSV6507 suspected by Luyten (1933a), NSV6446 and NSV6532 suspected by Luyten (1933b). Finding charts for these suspected variables have been never published.

Our studies are supported by grants from the Russian Foundation for Basic Research (grant No. 08-02-00375), from the Program "Origin and Evolution of Stars and Galaxies" of the Presidium of Russian Academy of Science, and from the Program of Support for Leading Scientific Schools of Russia (grant No. NSh 433.2008.2).

References:
Chen, Y.-T., Chen, W.-P., Hsiao, W.-S., Jiang, X., 2006, IBVS, No. 5700 (star No. 10)
Luyten, W.J., 1933a, AN, 249, 397
Luyten, W.J., 1933b, AN, 250, 260
Luyten, W.J., 1934, AN, 253, 136
Pojmanski, G., 2002, Acta Astronomica, 52, 397
Richter, G.A., 1970, Mitt. Veraend. Sterne, 5, 99
Wozniak, P.R., Vestrand, W.T., Akerlof, C.W. et al., 2004, Astron. J., 127, 2436



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