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arXiv 0811.3277astro-ph
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凌日系外行星的同质研究。II。物理性质

Homogeneous studies of transiting extrasolar planets. II. Physical properties

John Southworth

备注：
Accepted for publication in MNRAS (24 pages plus appendix, 9 figures and 24 tables)
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摘要：

我提出了一个均匀的测定的物理性质的14个过境的太阳系外行星系统，良好的数据。每个系统的输入量是光变曲线分析（论文1）的结果，以及已发表的恒星速度振幅Teff和[Fe/H]的测量结果。这些物理性质是通过在恒星理论的列表预测中插值确定的。统计不确定性使用扰动算法，它给出了一个详细的误差预算为每个输出量。通过比较使用不同恒星模型发现的值，评估每个量的系统不确定性。作为一个理论自由的替代方案，物理性质也计算使用经验的质量半径关系构造使用低质量食双星。行星的性质主要取决于从光和速度曲线测量的参数，对理论预测只有很小的敏感性。相比之下，轨道半长轴和恒星质量对理论预测有很强的依赖性，它们的系统不确定性可能比统计不确定性大得多。使用经验质量-半径关系代替，它们的值最多小15%。因此，我们对太阳系外行星的了解目前受到我们对低质量恒星缺乏了解的限制。使用所有已知的过境行星，我发现它们的轨道周期，质量和表面重力之间的相关性是显着的2-3西格玛水平。然而，根据它们的Safronov数将已知行星分为两类的分离比以前发现的要弱，并且可能在统计上不显着（删节）。

英文摘要：

I present an homogeneous determination of the physical properties of 14 transiting extrasolar planetary systems for which good data are available. The input quantities for each system are the results of the light curve analyses (Paper 1), and published measurements of the stellar velocity amplitude, Teff and [Fe/H]. The physical properties are determined by interpolating within tabulated predictions from stellar theory. Statistical uncertainties are found using a perturbation algorithm, which gives a detailed error budget for every output quantity. Systematic uncertainties are assessed for each quantity by comparing the values found using different stellar models. As a theory-free alternative, physical properties are also calculated using an empirical mass-radius relation constructed using low-mass eclipsing binary stars. The properties of the planets depend mostly on parameters measured from the light and velocity curves, and have only a minor sensitivity to theoretical predictions. In contrast, the orbital semimajor axes and stellar masses have a strong dependence on theoretical predictions, and their systematic uncertainties can be substantially larger than the statistical ones. Using the empirical mass--radius relation instead, their values are smaller by up to 15%. Thus our understanding of extrasolar planets is currently limited by our lack of understanding of low-mass stars. Using all known transiting planets, I find that correlations between their orbital periods, masses and surface gravities are significant at the 2-3 sigma level. However, the separation of the known planets into two classes according to their Safronov number is weaker than previously found, and may not be statistically significant (abridged).

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