Light elements for seven eclipsing binaries and for six suspected variables of other types

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

Received:   19.05.2021;   accepted:   28.05.2021
(E-mail for contact: helene@inasan.ru)

Comments:


1. Min II = 15.28 V.

2. Min II = 14.61 V, D = 0.04 P.

3. Min II = 13.96 V, D = 0.06 P. Twice longer period is also possible.

4. Min II = 13.22 V, D = 0.08 P. Min II – Min I = 0.645 P.

5. Near the position of NSV 14544 (Luyten, 1937). Variability of this star was discovered by us using Catalina Sky Survey (CRTS) photometric data.

6. Sp A1. Alias P = 0.711070 d.

7. Sp M4I. ASAS-SN photometry in V- and g-bands, taken together, was used for period determination. g magnitudes were corrected by –1 mag.

8. Min II = 10.95 V, D = 0.04 P. The star was suspected by Metzger (1931) who published no finding chart. Recovered by us using the ASAS-SN project photometric data.

9. J = 11.96, J – H = 0.40, H – K = 0.12. The star was suspected by Luyten (1935) who published no finding chart. Recovered by us using the Catalina Sky Survey (CRTS) photometric data.

10. Min II = 16.00 V. Min I may be Min II.

11. J = 11.17, J – H = 0.31, H – K = 0.24. The star was included in the ASAS-SN Catalog of Variable Stars (Jayasinghe et al. 2018) with a type SR and P = 109.3427086 d.

12. Min II = 15.54 V, D = 0.14 P. The star was included in the ASAS-SN Catalog of Variable Stars (Jayasinghe et al. 2018) with a type EB and P = 2.8822451 d.

13. Sp OB-. M – m = 0.33 P.

Remarks:
In the current paper, I continue to announce the preparation of the revised electronic version of the New catalogue of suspected variable stars (NSV). While working on compiling the next Name-List for Version 5.1 of the General Catalogue of Variable Stars (GCVS) (Samus et al. 2017), I determined types, light elements and improved coordinates for 1 new variable star and 12 stars towards the end of NSV catalogue (Kukarkin et al. 1982) to transfer them to the GCVS. The study of the variables was made using the publicly available electronic archive of CCD observations of the All-Sky Automated Survey for Supernovae (ASAS-SN) project (Shappee et al. 2014, Kochanek et al. 2017) and Catalina Sky Survey (CRTS) photometric data (Drake et al. 2009). To find periods I applied the WinEfk software provided by Dr. V.P. Goranskij and the online light curve analysis tool by Dr. K.V. Sokolovsky.

References:
Drake, A.J., Djorgovski, S.G., Mahabal, A., et al., 2009, Astrophys. J., 696, No. 1, 870
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