关于WY Cancri轨道周期变化的起源：一个真正的angular momentum损失？
On the origin of orbital period change in WY Cancri: a genuine angular momentum loss?
摘要：
巨蟹座WY是一颗短周期（$P$ =0.829 d）的食RS Canum Venaticorum星，两颗组成星都是晚型星。最近，由光度观测和光时极小值提供的观测结果表明，巨蟹座WY的轨道周期正以${\rm d} P/{\rm d}t=-1.2\times10^{-7}\rm d yr^{-1}$的速度经历长期减少。在这封信中，我们试图调查的周期变化的WY Cancri可以起源于角动量损失。在计算中，我们假设该源具有$\sim10^{-10} \rm M_{\odot} yr^{-1}$的高风损失率。为了解释观测结果，磁制动需要像Ap/Bp星一样的$\gtrsim 10000$ G强表面磁场。此外，如果这个源可能被环绕双星盘包围，并且6%的风损失供给盘，盘和双星之间的潮汐扭矩可以提供观测到的角动量损失率。如此强的磁场或极高的风输入分数似乎是极不可能的。
英文摘要：
WY Cancri is a short-period ($P$=0.829 d) eclipsing RS Canum Venaticorum stars, and both components are late-type stars. Recently, observations provided by photometric observations and light time minima show that the orbital period of WY Cancri is experiencing a secular decrease at a rate of ${\rm d} P/{\rm d}t=-1.2\times10^{-7}\rm d yr^{-1}$. In this Letter, we attempt to investigate if the period change of WY Cancri can originate from the angular momentum loss. In calculation, we assume that this source has a high wind loss rate of $\sim10^{-10} \rm M_{\odot} yr^{-1}$. To account for the observation, magnetic braking demands a strong surface magnetic field of $\gtrsim 10000$ G like Ap/Bp stars. Furthermore, if this source may be surrounded by a circumbinary disk, and 6% of the wind loss feeds the disk, tidal torque between the disk and the binary can offer the observed angular momentum loss rate. Such a strong magnetic field or an extremely high wind input fraction seem to be highly unlikely.
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