Types of Variability and Light Elements for 35 Suspected Variables from the NSV Catalog

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

Received:   22.04.2011;   accepted:   20.07.2011
(E-mail for contact: helene@inasan.ru, pastukhova@sai.msu.ru)

Comments:


2. M–m = 0.2P.

3. M–m = 0.34P.

5. M–m = 0.13P.

7. This star was discovered in the ASAS-3 survey and enters their variable-star catalog as a MISC/SR star but with a wrong period (207.0d).

9. This star was found, upon our request, by the late Dr. M. Hazen in Harvard Observatory's logbooks. No finding chart was available for this variable before.

10. This star was found, upon our request, by the late Dr. M. Hazen in Harvard Observatory's logbooks. No finding chart was available for this variable before.

11. M–m = 0.21:P.

12. MinII = 14.0.

13. R = 16.2 in the USNO Archive image of 1981.4962.

15. R = 15.2 in the USNO Archive image of 1984.2615.

16. R = 15.3 in the USNO Archive image of 1991.5852. The ASAS-3 range is for the combined brightness of the Mira and its neighbor.

19. R = 15.0 in the USNO Archive image of 1982.2587.

20. Not IRAS 16432–3139.

21. The ASAS-3 range is for the combined brightness of the Mira and its neighbor. This star was discovered in the ASAS-3 survey and enters their variable-star catalog as a MISC-type star but with a wrong period (41.8d). R = 10.7 in the USNO Archive image of 1991.5852 and R = 13.6 in the USNO Archive image of 1982.3313.

27. M–m = 0.38P.

29. MinII = 13.6. A twice shorter period and the DSCT type are possible.

31. This star was discovered by Sosna (1972) as a possible Mira-type variable.

33. R = 16.0 in the USNO Archive image of 1991.5934.

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

Remarks:
In our work aimed at improvement of the coordinates of variable stars in the NSV catalog (Samus et al. 2009), we checked a number of poorly studied variables and found new light elements and types for 35 of them. We recovered the variables NSV 07908, NSV 08121, NSV 08137 suspected by Luyten (1933); NSV 07899, NSV 07903, NSV 07925, NSV 07946, NSV 08000, NSV 08070, NSV 08084, NSV 08116 suspected by Luyten (1935); NSV 07561 suspected by Lampland (1914); NSV 07741 suspected by Leavitt (1904). Finding charts, light elements, and variability types for these suspected variables have never been published before. We could study the variables thanks to the publicly available electronic archives of CCD observations of the ASAS-3 project (Pojmanski 2002), ROTSE1/NSVS project (Wozniak et al. 2004), and to images of the US Naval Observatory Image and Catalog Archive.

Acknowledgments: Our studies are supported by a grant from the Program "Origin and Evolution of Stars and Galaxies" of the Presidium of Russian Academy of Sciences.

References:
Lampland, C.O., 1914, Astron. Nachr., 198, 351
Leavitt, H.S., 1904, Harvard Observ. Circ., 90, 1
Luyten, W.J., 1933, Astron. Nachr., 250, 259
Luyten, W.J., 1935, Astron. Nachr., 256, 325
Pojmanski, G., 2002, Acta Astron., 52, 397
Samus, N.N., Durlevich, O.V., et al., 2009, General Catalogue of Variable Stars, 2007–2011 (2009yCat....102025S)
Sosna, F.M., 1972, IBVS, No. 664
Wozniak, P.R., Vestrand, W.T., Akerlof, C.W., et al., 2004, Astron. J., 127, 2436