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首页> 外文期刊>The Astrophysical Journal. Supplement Series >Measurement of the spin-orbit misalignment of KOI-13.01 from its gravity-darkened Kepler transit lightcurve
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Measurement of the spin-orbit misalignment of KOI-13.01 from its gravity-darkened Kepler transit lightcurve

机译：从重力变暗的开普勒过渡光曲线测量KOI-13.01的自旋轨道未对准

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摘要

We model the asymmetry of the KOI-13.01 transit lightcurve assuming a gravity-darkened rapidly rotating host star in order to constrain the system's spin-orbit alignment and transit parameters. We find that our model can reproduce the Kepler lightcurve for KOI-13.01 with a sky-projected alignment of λ = 23° 4° and with the star's north pole tilted away from the observer by 48° 4° (assuming M * = 2.05 M _⊙). With both these determinations, we calculate that the net misalignment between this planet's orbit normal and its star's rotational pole is 56° ± 4°. Degeneracies in our geometric interpretation also allow a retrograde spin-orbit angle of 124° ± 4°. This is the first spin-orbit measurement to come from gravity darkening and is one of only a few measurements of the full (not just the sky-projected) spin-orbit misalignment of an extrasolar planet. We also measure accurate transit parameters incorporating stellar oblateness and gravity darkening: R _* = 1.756 ± 0.014 R_⊙, R _p = 1.445 ± 0.016 R_(Jup), and i = 859 04. The new lower planetary radius falls within the planetary mass regime for plausible interior models for the transiting body. A simple initial calculation shows that KOI-13.01's circular orbit is apparently inconsistent with the Kozai mechanism having driven its spin-orbit misalignment; planet-planet scattering and stellar spin migration remain viable mechanisms. Future Kepler data will improve the precision of the KOI-13.01 transit lightcurve, allowing more precise determination of transit parameters and the opportunity to use the Photometric Rossiter-McLaughlin effect to resolve the prograde/retrograde orbit determination degeneracy.
机译：我们假设重力变暗的快速旋转的宿主恒星对KOI-13.01过渡光曲线的不对称进行建模，以约束系统的自旋轨道对准和过渡参数。我们发现我们的模型可以重现KOI-13.01的开普勒光曲线，其天空投影对准线为λ= 23°4°，并且恒星的北极偏离观察者48°4°（假设M * = 2.05 M _⊙）。通过这两个确定，我们计算出该行星的轨道法线与其恒星的旋转极之间的净错位为56°±4°。在我们的几何解释中，简并性还允许逆行自旋轨道角为124°±4°。这是来自重力变暗的第一个自旋轨道测量，并且是对太阳系外行星的完整（不仅是天空投影）自旋轨道未对准的少数测量之一。我们还测量了结合了恒星扁度和重力变暗的准确的过渡参数：R _ * = 1.756±0.014R_⊙，R _p = 1.445±0.016 R_（Jup）和i = 85904。新的下行星半径位于行星质量之内合理的过境车身内部模型制度。一个简单的初始计算表明，KOI-13.01的圆形轨道显然与驱动其自旋轨道未对准的Kozai机制不一致。行星行星散射和恒星自旋迁移仍然是可行的机制。未来的开普勒数据将提高KOI-13.01过渡光曲线的精度，从而可以更精确地确定过渡参数，并有机会使用光度Rossiter-McLaughlin效应来解决前进/后退轨道确定的简并性。

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