Article in PDF |
"Peremennye Zvezdy", Prilozhenie, vol. 8, N 40 (2008) |
ISSN 2221–0474 |
Received: 12.09.2008; accepted: 13.11.2008
(E-mail for contact: khruslov@bk.ru)
|
Comments:
1. MinII = 15.3. The ROTSE data with photometric correction flags (usually rejected) were kept for the analysis.
2. MinII = 14.15. Period P = 0.2750 d is not excluded.
3. MinII = 13.6.
4. MinII = 14.6.
5. MinII = 14.2.
6. MinII = 12.4.
7. MinII = 14.15.
8. MinII = 13.3.
9. MinII = 13.6:.
10. MinII = 13.85. The ROTSE data with photometric correction flags (usually rejected) were kept for the analysis.
11. MinII = 13.85.
12. MinII = 13.9. The ROTSE data with photometric correction flags (usually rejected) were kept for the analysis.
13. MinII = 13.65.
14. MinII = 12.6.
15. MinII = 14.6.
16. MinII = 11.05.
17. MinII = 13.0.
18. MinII = 10.93. Type ELL is not excluded. X-ray source 1RXS J012947.3+330349.
19. MinII = 13.75:.
20. MinII = 14.05. The ROTSE data with photometric correction flags (usually rejected) were kept for the analysis.
21. MinII = 14.6. The ROTSE data with photometric correction flags (usually rejected) were kept for the analysis.
22. MinII = 14.45. The ROTSE data with photometric correction flags (usually rejected) were kept for the analysis.
23. MinII = 14.3. D = 0.10P. The RS-type variability in maximum brightness is possible.
24. MinII = 14.3:.
25. MinII = 14.2. The ROTSE data with photometric correction flags (usually rejected) were kept for the analysis.
26. MinII = 13.2. The ROTSE data with photometric correction flags (usually rejected) were kept for the analysis.
27. MinII = 14.5:. The ROTSE data with photometric correction flags (usually rejected) were kept for the analysis.
28. MinII =12.65. Very close pair of stars of similar brightness: 2MASS 01530806+3116012 and 2MASS 01530782+3115584. It is not possible to choose which star of the pair is variable. The amplitude of variability is underestimated.
29. MinII = 14.4.
30. MinII = 14.8.
31. MinII = 14.7. The ROTSE data with photometric correction flags (usually rejected) were kept for the analysis.
32. MinII = 13.6.
33. MinII = 12.07.
34. Independent discovery of variability. The period in Hoffman et al. (2008), P = 0.55711, is wrong. MinII = 13.4.
35. MinII = 14.1.
36. MinII = 13.7. Type EA is not excluded, D = 0.11P. The ROTSE data w ith photometric correction flags (usually rejected) were kept for the analysis.
37. MinII = 14.6. The ROTSE data with photometric correction flags (usually rejected) were kept for the analysis.
38. MinII = 14.6.
39. MinII = 14.4. The ROTSE data with photometric correction flags (usually rejected) were kept for the analysis.
40. MinII =13.2.
41. MinII = 15.1. The ROTSE data with photometric correction flags (usually rejected) were kept for the analysis.
42. MinII = 14.7.
43. MinII = 13.3.
44. MinII = 14.2. The ROTSE data with photometric correction flags (usually rejected) were kept for the analysis.Remarks:
I present the discovery of 44 new short-period eclipsing binaries (mostly EW). 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:
Hoffman, D.I., Harrison, T.E., Coughlin, J.L. et al., 2008, Astron. J., 136, 1067
Wozniak, P.R., Vestrand, W.T., Akerlof, C.W. et al., 2004, Astron. J., 127, 2436