Article in PDF |
"Peremennye Zvezdy", Prilozhenie, vol. 8, N 51 (2008) |
ISSN 2221–0474 |
Received: 5.12.2008; accepted: 10.12.2008
(E-mail for contact: helene@inasan.ru, pastukhova@sai.msu.ru)
|
Comments:
1. USNO-A2.0: R = 15.7.
3. USNO-B1.0: R = 15.6.
5. USNO-A2.0: R = 15.4. The ASAS-3 range is for the combined brightness of the Mira and its neighbor.
6. 11.7 - 15.7 pg in Luyten (1933b). The ASAS-3 range is for the combined brightness of the Mira and its neighbor.
8. 13.5 - <15.5 pg in Luyten (1933b), USNO-A2.0: B = 17.8. The ASAS-3 range is for the combined brightness of the Mira and its neighbor.
9. NSV 6743 = NSV 20142. According to Luyten (1934), 13.3-16 pg. Luyten's star was found, upon our request, by D. Williams and M. Hazen on Harvard plates. Independently announced by Grayzeck (1978) who published a finding chart but gave a declination wrong by one degree, resulting in the second NSV entry. R = 14.0 on the Aladin image of March 11, 1997. The ASAS-3 range is for the combined brightness of the Mira (GSC 8691-02470) and two its neighbors, a red star GSC 8691-01638 and a bright companion GSC 8691-02468. P = 222d in the ASAS-3 variable-star catalog (Pojmanski 2002).
10. R = 15.4 on the USNO Archive image of June 20, 1993. The ASAS-3 range is for the combined brightness of the Mira and its neighbor.
18. R = 14.0 on the USNO Archive image of July 16, 1991. The ASAS-3 range is for the combined brightness of the Mira and its neighbor.
19. USNO-A2.0: R = 16.6.
21. The ASAS-3 range is for the combined brightness of the Mira and its neighbor.
22. The ASAS-3 range is for the combined brightness of the Mira and its close neighbor.
23. USNO-A2.0: R = 15.8.
24. USNO-A2.0: R = 15.5.
25. 14.5 - <18 pg in Luyten (1934).
26. USNO-A2.0: R = 16.4.
29. The ASAS-3 range is for the combined brightness of the Mira and its neighbor.Remarks:
We could study the variables thanks to the publicly available electronic archives of CCD observations of the ASAS-3 project (Pojmanski, 2002) and to images of the US Naval Observatory Image and Catalogue Archive (http://www.nofs.navy.mil/data/FchPix/). We recovered the variables NSV 06641, NSV 06705, NSV 06752 suspected by Luyten (1933a); NSV 06658, NSV 06751, NSV 06771, NSV 06774, NSV 06830 suspected by Luyten (1935); NSV 06650, NSV 06730, NSV 06743, NSV 06780, NSV 06805, NSV 06835, NSV 06843, NSV 06864, NSV 06896 suspected by Luyten (1934); NSV 06731, NSV 06734, NSV 06740, NSV 06802, NSV 06803, NSV 06809 suspected by Luyten (1933b). Finding charts for these suspected variables have never been published.
Acknowledgments: 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.References:
Grayzeck, E.J., 1978, Astron. J., 83, 1390
Luyten, W.J., 1933a, AN, 249, 395
Luyten, W.J., 1933b, AN, 250, 259
Luyten, W.J., 1934, AN, 253, 135
Luyten, W.J., 1935, AN, 256, 325
Pojmanski, G., 2002, Acta Astronomica, 52, 397