Issue |
A&A
Volume 387, Number 3, June I 2002
|
|
---|---|---|
Page(s) | 903 - 906 | |
Section | Interstellar and circumstellar matter | |
DOI | https://doi.org/10.1051/0004-6361:20020167 | |
Published online | 17 May 2002 |
BO Pegasi: A candidate on the breaking stage of the TRO cycle
Yunnan Observatory, Chinese Academy of Sciences, PO Box 110, 650011 Kunming, PR China National Astronomical Observatories, Chinese Academy of Science (NAOCAS) United Laboratory of Optical Astronomy, Chinese Academy of Science (ULOAC)
Corresponding author: qsb@netease.com
Received:
5
June
2001
Accepted:
28
January
2002
A detailed period study of the short-period () close
binary system, BO Peg, is presented based on the analysis of its O–C curve.
It is found that the orbital period shows a continuous decrease
with a rate dP/dt
days/year while it
undergoes a possible small-amplitude oscillation.
If the period oscillation is cyclic, it can be explained
either by the light-time effect via the presence of an unseen third body
or by the magnetic activity cycle of the secondary component.
The continuous period decrease suggests a secular mass transfer from the
more massive to the less massive component, which is in agreement
with the near-contact configuration with a lobe-filling primary
(Yamasaki & Okazaki [CITE]). These
observations, as seen in RT Scl, FT Lup, TT Her, RS Ind,
and V388 Cyg, are consistent with the Thermal Relaxation Oscillation
(TRO) theory in that the primary component is transferring
mass to the secondary in the broken-contact phase. To satisfy such a
decrease in the orbital period, a conservative mass transfer rate
(with no magnetic effect) would be of the order of
dM/dt
.
Key words: stars: binaries: close / stars: individuals: BO Peg / stars: evolution
© ESO, 2002
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