New Period Investigation of Algol-like Near-Contact Binary EG Cephei

Details New Period Investigation of Algol-like Near-Contact Binary EG Cephei New Period Investigation of Algol-like Near-Contact Binary EG Cephei

Jun 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009pasj...61..529z&link_type=abstract

Publications of the Astronomical Society of Japan, Vol.61, No.3, pp.529--533

Astronomy and Astrophysics

Astronomy

2

Stars: Binaries: Eclipsing, Stars: Evolution, Stars: Individual (Eg Cephei)

Scientific paper

The Algol-like Near Contact Binary EG Cephei was observed in 2008 October. One new observed time of the secondary minimum was derived in BV(IR)c bands. It turns out that the times of minima at longer wavelengths occur earlier than the shorter ones. All of the available eclipse times, including 735 epochs, spanning more than 100 years were analyzed. A period oscillation with a period of 35.8(±0.1)yr and an amplitude of about 0.0037(±0.0002)d was found, while undergoing a secular increase at a rate of dP/dt = 3.4 × 10-8 (±0.1)d yr-1. This continuous period increase may be caused by mass transfer from the secondary component to the primary one on a thermal timescale, which is consistent with the Algol-like semi-detached configuration of EG Cep. Combining with the spectroscopic and photometric results, we derived a conservative mass-transfer rate of this target, dM/dt = 3.0(±0.1) × 10-8Modotyr-1. The oscillation part of the period variation may be the result of a light-time effect due to the existence of a coplanar additional body with a mass of M3 = 0.11Modot, and a corresponding radius of a3 = 14AU. The presumed third body may play an important role in the evolution of this system.

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