Article in PDF |
"Peremennye Zvezdy", Prilozhenie, vol. 14, N 9 (2014) |
ISSN 2221–0474 |
Received: 7.06.2013; accepted: 29.05.2014
(E-mail for contact: helene@inasan.ru, pastukhova@sai.msu.ru)
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Comments:
1. R = 15.7 on the SERC-DSS2 image of 1998-06-17.
3. R = 14.5 on the SERC-DSS2 image of 1989-09-03.
5. R = 16.5 on the SERC-DSS2 image of 1997-03-31.
6. The ASAS-3 range is for the combined brightness of the Mira and its neighbor. R = 15.5 on the ESO-MAMA image of 1985-04-25.
7. R = 16.3 on the ESO-MAMA image of 1985-06-26.
8. The ASAS-3 range is for the combined brightness of the Mira and its neighbor. R = 16.0 on the SERC-DSS2 image of 1996-09-06.
9. R = 16.1 on the AAO-DSS2 image of 1992-07-22.
10. Woźniak et al. (2004) give a wrong period (280 d) for this Mira star.
12. R = 17.0 on the SERC-DSS2 image of 1989-09-03.
13. R = 16.9 on the SERS-DSS2 image of 1996-09-06.
14. R = 16.5 on the AAO-DSS2 image of 1992-08-01.
15. R = 17.0 on the AAO-DSS2 image of 1992-08-01.
16. R = 15.6 on the AAO-DSS2 image of 1992-07-22.
17. HV 9499 was discovered by Luyten (1935). We assume that there was a misprint in the published declination: –46°49′ instead of the correct value of –47°49′.
18. R = 16.5 on the SERC-DSS2 image of 1997-03-31.
20. R = 16.8 on the AAO-DSS2 image of 1990-06-22.
21. The ASAS-3 range is for the combined brightness of the Mira and its neighbor. R = 16.6 on the SERC-DSS2 image of 1996-09-06.
22. R = 16.9 on the AAO-DSS2 image of 1993-04-18.
23. The ASAS-3 range is for the combined brightness of the Mira and its neighbor. SRA type is possible.
24. R = 14.9 on the AAO-DSS2 image of 1991-09-06.
25. We have got only one maximum in ASAS-3 for this star and 5 our measurements in R band (USNO Archive):
JD R 2438560 14.7 2444476 17.0 2447774 17.0 2448506 15.0 2450334 17.4
26. The ASAS-3 range is for the combined brightness of the Mira and its neighbor. R = 16.0 on the SERC-DSS2 image of 1996-09-06.
27. R = 16.2 on the SERC-DSS2 image of 1996-09-07.
28. R = 16.0 on the SERS-DSS2 image of 1996-09-06.
29. R = 16.4 on the ESO-MAMA image of 1980-08-23.
30. R = 16.5 on the SERC-DSS2 image of 1986-08-16.
31. The ASAS-3 range is for the combined brightness of the Mira and its neighbor. R = 17.0 on the SERC-DSS2 image of 1987-09-16.
32. R = 16.2 on the SERS-DSS2 image of 1996-09-07.
33. R = 15.5 on the SERS-DSS2 image of 1996-09-13.
34. R = 16.0 on the ESO-MAMA image of 1984-04-23.
35. R = 15.5 on the SERC-DSS2 image of 1998-07-16.
36. R = 16.7 on the ESO-MAMA image of 1978-01-07.
37. R = 15.0 on the ESO-MAMA image of 1985-07-15.Remarks:
In our work aimed at improvement of the coordinates of variable stars in the NSV catalog (Samus et al. 2007–2013), we determined new light elements for 37 Mira type stars. The variables were studied using data from the publicly available electronic archives of CCD observations of the ASAS-3 project (Pojmanski 2002), and images from the US Naval Observatory Image and Catalog Archive. HV 8740, HV 8743, HV 8754, HV 9091, HV 8764, HV 8767, and HV 9119 were found, upon our request, by D. Williams on Harvard plates and HV 6584 was found, upon our request, by the late Dr. M. Hazen in Harvard Observatory's logbooks. The other 29 stars were rediscovered by the authors.
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 and by the Russian Foundation for Basic Research grant 13-02-00664.References:
Luyten, W.J., 1935, Astron. Nachr., 256, 325
Pojmanski, G., 2002, Acta Astron., 52, 397
Samus, N.N., Durlevich, O.V., Goranskij V.P., Kazarovets, E.V., Kireeva, N.N., Pastukhova E.N., Zharova A.V., 2007–2013, General Catalogue of Variable Stars, Centre de Données Astronomiques de Strasbourg, B/gcvs
Woźniak, P.R., Williams, S.J., Vestrand, W.T., Gupta, V., 2004, Astron. J., 128, 2965