40 Red Variable Stars: Variability Types and Light Elements

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

Received:   28.12.2015;   accepted:   29.04.2016
(E-mail for contact: Institute of Astronomy, Russian Academy of Sciences, Moscow, Russia)

Comments:


3. Variability was discovered in the ASAS-3 survey; the star enters their variable-star catalog as a MISC-type star with a wrong period of 192^d.7.

4. Superposed variations of P = 95^d.5. HV 7220 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.

12. The ASAS-3 range is for the combined brightness of the variable star and its neighbor. Variable is the SE component of 4" pair. Mira type for this variable is not excluded.

13. One well-defined maximum (JD = 2431620) observed by Hoffleit (1964) was used to improve our elements.

15. Superposed variations of P = 48^d.0. Variability was discovered in the ASAS-3 survey; the starenters their variable-star catalog as a MISC-type star with a wrong period of 168^d.5.

16. HV 9890 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.

17. Variability was discovered in the ASAS-3 survey; the star enters their variable-star catalog as a MISC-type star with a wrong period of 122^d.2.

18. Superposed variations of P = 52^d.3. Variability was discovered in the ASAS-3 survey; the star enters their variable-star catalog as a MISC-type star with a wrong period of 63^d.4.

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

23. Variability was discovered in the ASAS-3 survey; the star enters their variable-star catalog as a MISC-type star with a wrong period of 180^d.

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

28. Variability was discovered in the ASAS-3 survey; the star enters their variable-star catalog as a MISC-type star with a wrong period of 183^d.7.

29. Variability was discovered in the ASAS-3 survey; the star enters their variable-star catalog as a MISC-type star with a wrong period of 142^d.1.

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

32. Variability was discovered in the ASAS-3 survey; the star enters their variable-star catalog as a MISC-type star with a wrong period of 41^d.6.

35. We study the variability of NSV 11371 using the Northern Sky Variability Survey (NSVS) unfiltered data (Woźniak et al. 2004a), but epoch of maximum brightness used is from the online publicly available Catalina Sky Survey data (2013) for CSS J184818.4+401757.

36. This star, NSVS J1849573+203211, was studied by Woźniak et al. (2004b), they gave the Mira type and a wrong period of 282^d.

40. Variability was discovered in the ASAS-3 survey; the star enters their variable-star catalog as a MISC-type star with a wrong period of 175^d.3.

Remarks:
As a part of our work on improvement of coordinates of variable stars in the NSV catalog (Samus et al. 2007–2015), we derived light elements and types for 40 red stars. We recovered the following variables suspected by W.J. Luyten: HV 9459, HV 9464, HV 9477, HV 9499, and HV 9518 (Luyten 1937); HV 9465 (Luyten 1935); HV 9454 and HV 9506 (Luyten 1936); and also the stars Innes 59 suspected by Innes (1914) and BV 813 suspected by Strohmeier et al. (1966). We measured minimal brightness for many Mira variables in Digitized Sky Survey images (R-band). We studied the variables using the publicly available electronic archives of CCD observations of the ASAS-3 project (Pojmanski 2002), and images of the STScI and US Naval Observatory Image and Catalog Archive. We found and investigated four new long-period variable stars: 2MASS 17433740-4043165, 2MASS 18063887-4137025, 2MASS 18092874-3407406, and GSC 9055-02486.

Acknowledgments: Our studies are supported by a grant from the Program "Transition and explosive processes in the Universe" of the Presidium of Russian Academy of Sciences.

References:
Hoffleit, D., 1964, Astron. J., 69, 301
Innes, R., 1914, Circ. Union Obs., No. 20
Luyten, W.J., 1935, Astron. Nachr., 256, 325
Luyten, W.J., 1936, Astron. Nachr., 258, 121
Luyten, W.J., 1937, Astron. Nachr., 261, 451
Pojmanski, G., 2002, Acta Astron., 52, 397
Samus, N.N., Durlevich, O.V., Goranskij, V.P., Kazarovets, E V., Kireeva, N.N., Pastukhova, General Catalogue of Variable Stars, Centre de Données Astronomiques de Strasbourg, B/gcvs
Strohmeier, W., Fischer, H., Ott, H., 1966, Inform. Bull. Var. Stars, No. 140
Woźniak, P.R., Vestrand, W.T., Akerlof, C.W., et al., 2004a, Astron. J., 127, 2436
Woźniak, P.R., Williams, S.J., Vestrand, W.T., Gupta, V., 2004b, Astron. J., 128, 2965