行星对宿主恒星形状的影响-牧夫座τ的椭球变化
Planet influence on the shape of the hosting star - ellipsoidal variations of tau Bootis
摘要：
本文用Wilson-Devinney方法测量被近距离大质量行星畸变的恒星的亮度，估计了探测椭球变化的可能性。Phafl et al.（2008）和Loeb and Gaudi（2003）已经讨论过这个问题。这种效应在双星的情况下是众所周知的，它可以产生光变曲线，对于扭曲的恒星，椭圆变化的振幅约为0.1等。对于行星来说，这种影响非常小，通常小于0.0001 mag. The检测的系外行星，通过寻找小振幅的椭球变化，将是非常困难的，并受到其他光度效应的影响;然而，它可能在一些极端的情况下。椭球变化的观测可以对系统模型提供额外的约束。用基于Wilson-Devinney方法的PHOEBE食双星软件计算了几个恒星/行星系统的光变曲线。作为一个例子的椭圆形变化的合成光变曲线的牧夫座τ。椭球变化幅度为0.01毫等。这颗伴星是质量为7.3 Mjup的短周期热木星。
英文摘要：
This paper presents estimations on the possibility of detection of ellipsoidal variations by means of measuring brightness of the star distorted by a close massive planet using Wilson-Devinney method. The problem was already discussed by Phafl et al. (2008) and earlier by Loeb and Gaudi (2003). The effect is well known in the case of binary stars where it can produce light curves with amplitutudes of ellipsoidal variations of about 0.1 mag for distorted stars. For planets the effect is very small and usually less than 0.0001 mag. The detection of an exoplanet, by searching for small amplitude ellipsoidal variations, will be very difficult and affected by other photometric effects; however, it maybe possible for some extreme cases. Observations of ellipsoidal variations can provide additional constraints on the model of the system. Light curves for few star/planet systems have been calculated using PHOEBE eclipsing binary software based on Wilson-Devinney method. As an example of ellipsoidal variations the synthetic light curve for tau Bootis is presented. The amplitude of ellipsoidal variation is 0.01 mmag. The companion is massive 7.3 Mjup and short-period hot Jupiter.
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