Article in PDF |
"Peremennye Zvezdy", Prilozhenie, vol. 11, N 1 (2011) |
ISSN 2221–0474 |
Received: 3.10.2010; accepted: 19.01.2011
(E-mail for contact: khruslov@bk.ru)
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Comments:
1. MinII = 14.0. The ROTSE data with photometric correction flags (usually rejected) were kept for the analysis.
2. MinII = 14.6. The ROTSE data with photometric correction flags (usually rejected) were kept for the analysis.
3. MinII = 12.45. The star has a faint close companion 2MASS 02064073+3343231. The ROTSE data with photometric correction flags (usually rejected) were kept for the analysis.
4. MinII = 14.1. Perhaps a blend of two stars, GSC 2339-00364 and GSC 2339-00223, in the NSVS. The variability amplitude can be underestimated. The ROTSE data with photometric correction flags (usually rejected) were kept for the analysis.
5. MinII = 14.7.
6. MinII = 14.3.
7. MinII = 13.05. The ROTSE data with photometric correction flags (usually rejected) were kept for the analysis.
8. MinII = 12.7. All observations with correction flag 50 were rejected.
9. MinII = 12.97.
10. MinII = 13.3.
11. MinII = 14.2.
12. BD+47 2107. The system's mean brightness varies. The ROTSE data with photometric correction flags (usually rejected) were kept for the analysis.
13. MinII = 15.3:.
14. MinII = 14.5:. Period P = 0.347172 days is not excluded. The ROTSE data with photometric correction flags (usually rejected) were kept for the analysis.
15. MinII = 14.4:.
16. MinII = 13.1. The ROTSE data with photometric correction flags (usually rejected) were kept for the analysis.
17. MinII = 11.24. X-ray source 1RXS J150615.9+564111. ELL type is possible.
18. MinII = 13.9, D = 0.13 P. The ROTSE data with photometric correction flags (usually rejected) were kept for the analysis.
19. HD 143775, BD+61 1552. MinII = 10.43. A twice shorter period and type RRC are possible. The ROTSE data with photometric correction flags (usually rejected) were kept for the analysis.
20. MinII = 14.25. The ROTSE data with photometric correction flags (usually rejected) were kept for the analysis.
21. There is a faint close companion. A twice longer period is possible. The ROTSE data with photometric correction flags (usually rejected) were kept for the analysis.
22. MinII = 14.6:. EA type is not excluded. The ROTSE data with photometric correction flags (usually rejected) were kept for the analysis.
23. MinII = 14.45.
24. MinII = 13.51. The colour index J–H = 0.103 (2MASS) is in agreement with EB type. The ROTSE data with photometric correction flags (usually rejected) were kept for the analysis.
25. MinII = 14.9.
26. MinII = 14.5. D = 0.18 P. EW type is not excluded. The ROTSE data with photometric correction flags (usually rejected) were kept for the analysis.
27. MinII = 13.9. Slight O'Connell effect. The ROTSE data with photometric correction flags (usually rejected) were kept for the analysis.
28. MinII = 15.1. The ROTSE data with photometric correction flags (usually rejected) were kept for the analysis.
29. MinII = 14.5. The ROTSE data with photometric correction flags (usually rejected) were kept for the analysis.
30. MinII = 14.8. The ROTSE data with photometric correction flags (usually rejected) were kept for the analysis.
31. MinII = 14.7. The ROTSE data with photometric correction flags (usually rejected) were kept for the analysis.
32. MinII = 14.35. The ROTSE data with photometric correction flags (usually rejected) were kept for the analysis.
33. MinII = 13.65. D = 0.14 P. The ROTSE data with photometric correction flags (usually rejected) were kept for the analysis.Remarks:
I present the discovery of 33 new short-period (mostly EW) eclipsing binaries. A search for variables was carried out in the publicly available data of the Northern Sky Variability Survey (NSVS, Wozniak et al. 2004, also see http://skydot.lanl.gov/nsvs). These observations were analyzed using the period-search software developed by Dr. V.P. Goranskij for Windows environment. The coordinates were drawn either from the Tycho-2 or 2MASS catalogs.References:
Wozniak, P.R., Vestrand, W.T., Akerlof, C.W., et al., 2004, Astron. J., 127, 2436