|
Peremennye Zvezdy (Variable Stars) 28, No. 4, 2008 Received 15 February; accepted 20 March.
|
Article in PDF |
Pulsations in the Eclipsing Binary NSV 10993
A.V. Khruslov
Tula, Russia; e-mail: khruslov@bk.ru
| I present the discovery of a pulsating component in light variations of the known eclipsing binary NSV 10993 based on the NSVS and ASAS-3 publicly available data. |
The variability of NSV 10993 = S 4320 = GSC 1032-01378 was
discovered by Hoffmeister (1949). Later the star was
re-investigated by Götz & Wenzel (1956). In both papers, their
authors ascribe the variable to eclipsing binaries, possibly to
the W UMa stars. According to Otero & Wils (2005), NSV 10993 is
an EA eclipsing binary with the elements:
The study of the last cited authors was based on the NSVS (Wozniak et al., 2004) and ASAS-3 (Pojmanski, 2002) publicly available data. The light curve they published shows a scatter quite unusual for a not too faint star, suggesting a possibility of additional periodic or aperiodic components in the variations.
I re-analysed the NSVS and ASAS-3 data (NSVS 10974803, NSVS
11094130, and ASAS 183213+1217.1) using the WINEFK package by
Dr. V.P. Goranskij and found pulsations superposing the eclipsing
light curve. The light elements of the eclipsing and pulsating
components of the light variations are the following:
and
The corresponding light curves based on the NSVS observations are shown in the Figure. The pulsating light curve is asymmetric,
. The eclipsing light curve is similar to the EB-type
curves. The ASAS-3 data do not contradict the proposed
interpretation. The variability ranges are 12
6-132 (
,
NSVS) and 1255-1305 (
, ASAS-3).
From these results, we may consider the system as a good candidate to eclipsing binaries with a Cepheid component, similar to the recently discovered variable TYC 1031 01262 1 (Antipin et al., 2007).
 |
Fig. 1. The phased light curves for eclipsing and pulsating components of the light variations. The top panels are based on the original NSVS observations, the bottom panels are constructed for deviations from the mean light curve of the other periodicity. |
Acknowledgements: The author is grateful to Dr. V.P. Goranskij for providing software for the light-curve analysis. Thanks are due to Drs. S.V. Antipin and N.N. Samus for helpful discussions.
References:
Antipin, S.V., Sokolovsky, K.V., Ignatieva, T.I., 2007, MNRAS, 379, L60
Hoffmeister, C., 1949, Ergänzungshefte Astron. Nachrichten, 12, No.1
Götz, W., Wenzel, W., 1956, Veröff. Sternw. Sonneberg, 2, H.5
Otero, S., Wils, P., 2005, IBVS, No. 5644
Pojmanski, G., 2002, Acta Astronomica, 52, 397
Wozniak, P.R., Vestrand, W.T., Akerlof, C.W. et al., 2004, Astron. J., 127, 2436