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首页> 外文期刊>PASJ: Publications of the Astronomical Society of Japan >On the Origin of Orbital Period Change in WYCancri: A Genuine Angular-Momentum Loss?
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On the Origin of Orbital Period Change in WYCancri: A Genuine Angular-Momentum Loss?

机译：关于WYCancri轨道周期变化的起源：真正的角动量损失？

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摘要

WYCnc is a short-period (P = 0.829 d) eclipsing RS Canum Venaticorum star, and both components are of the late-type stars. Recently, observations provided by photometric observations and light-time minima show that the orbital period of WYCnc is experiencing a secular decrease at a rate of dP/dt = -1.2 × 10~(-7) dyr~(-1). In this letter, we consider whether the period change of WYCnc can originate from angular-momentum loss. In calculations, we assumed that this source has a high wind loss rate of ~10~(10)M_☉ yr~(-1). To account for the observation, magnetic braking demands a strong surface magnetic field of greater, similar 10000 G, like that of Ap/Bp stars. Furthermore, if this source is perhaps surrounded by a circumbinary disk, and 6% of the wind loss feeds the disk, the tidal torque between the disk and the binary can account for the observed angular-momentum loss rate. Such a strong magnetic field, or an extremely high wind input fraction, seems to be highly unlikely.
机译：WYCnc是一个短周期（P = 0.829 d），超过了RS Canum Venaticorum星，这两个分量都是晚型星。近来，由光度学观测和光时间最小值所提供的观测表明，WYCnc的轨道周期正以dP / dt = -1.2×10〜（-7）dyr〜（-1）的速率经历长期下降。在这封信中，我们考虑了WYCnc的周期变化是否可以源自角动量损失。在计算中，我们假设此风源的风损率很高，约为10〜（10）M_☉yr〜（-1）。为了说明这一点，与Ap / Bp星一样，电磁制动需要更大的强表面磁场，类似于10000G。此外，如果此源可能被外接圆盘围绕，并且有6％的风损耗馈入圆盘，则圆盘和双星之间的潮汐扭矩可以说明观测到的角动量损耗率。如此强的磁场或极高的风输入比似乎不太可能。

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