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Astron. Astrophys. Suppl. Ser. 146, 377-384

Long-time behavior of orbital periods of some Algol-type eclipsing binaries[*]

Qian Shengbang1,2,3

Send offprint request: Qian Shengbang

1 - Yunnan Observatory, Chinese Academy of Sciences, P.O. Box 110, 650011 Kunming, PR China
2 - National Astronomical Observatories, Chinese Academy of Science (NAOCAS), PR China
3 - United Laboratory of Optical Astronomy, Chinese Academy of Science (ULOAC), PR China

Received May 2; accepted July 19, 2000


Orbital period variations of six semi-detached binaries, UW Cyg, RX Hya, AK Ser, AC Tau, UW Vir and VV Vul, are presented based on the analysis of their O-C observations. For AK Ser and VV Vul, their orbital periods may show secular increase at rates of ${\rm d}P/{\rm d}t=+7.94\ {10^{-7}}$ and $+3.43\
{10^{-6}}$ days/year. For UW Cyg, its orbital period is revised, and the O-C curve shows a cyclic variation with a period of 49.2years and an amplitude of $0\hbox{$.\!\!^{\rm d}$ }0383$. For the other three systems, RX Hya, AC Tau and UW Vir, the changes in their orbital periods appear more complex but their O-C curves can be represented by periodic variations (with periods of 54.3, 29.8 and 45.9years) superimposed on upward parabolic segments. The components of upward curving parabolic variations in RX Hya, AC Tau and UW Vir indicate secular period increase with rates of ${\rm d}P/{\rm d}t=+1.04\ {10^{-6}}$, $+7.11\ {10^{-7}}$ and $+1.73\ {10^{-6}}$ days/year respectively. The secular period increase in the five systems, RX Hya, AK Ser, AC Tau, UW Vir and VV Vul, can be explained by mass transfer from the less to the massive components, which is consistent with their semi-detached configurations. The periodic changes of the orbital periods in UW Cyg, RX Hya, AC Tau, UW Vir may be caused by the light-time effects due to the existence of the third bodies.

Key words: stars: individuals: UW Cyg, RX Hya, AK Ser, AC Tau, UW Vir and VV Vul

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