System Parameters of the Transiting Extrasolar Planet HD 209458b
System Parameters of the Transiting Extrasolar Planet HD 209458b
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DOI：
10.1086/433176
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发表时间：
2005-04
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通讯作者：
R. Wittenmyer;R. Wittenmyer;W. Welsh;J. Orosz;A. Schultz;W. Kinzel;M. Kochte;F. Bruhweiler;D. Bennum;G. Henry;Geoffrey W Marcy;Debra A. Fischer;R. P. Butler;S. Vogt
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作者：
R. Wittenmyer;R. Wittenmyer;W. Welsh;J. Orosz;A. Schultz;W. Kinzel;M. Kochte;F. Bruhweiler;D. Bennum;G. Henry;Geoffrey W Marcy;Debra A. Fischer;R. P. Butler;S. Vogt
我们使用一个同时符合光度中转和径向速度观测的模型，推导出HD 209458系统的改进的系统参数。光度测量包括以前的哈勃空间望远镜STI和FGS观测，2001年至2003年用拉古纳山天文台1米望远镜观测的12个I波段凌日，以及2001年至2004年用费尔伯恩天文台的两个自动光度望远镜观测的6个斯特伦格伦b+y凌日。径向速度是由Keck Hires观测得到的。该模型适当地处理了系统的轨道动力学，从而产生了健壮的和物理上自洽的解。我们的一组系统参数与以前发表的结果一致，尽管精度有所提高。例如，对0.93-1.20M☉的恒星质量施加稳健的限制，我们得到1.26RJ；1.42RJ和0.59MJ<；0.70MJ。我们可以通过包括恒星质量-半径关系约束来减少这些估计的不确定性，产生RPlanet=Rj和MPlanet=Mj。我们的结果证实，行星半径比辐射行星演化模型预测的大10%-20%，证实了需要额外的机制来减缓行星的进化收缩。得到了一个修正的星历，T0=2,452,854.82545+3.52474554E(HJD)，该星历现在包含了S 0.016年间的不确定性，应该有助于今后在HD 209458系统中寻找行星卫星和其他天体。
We derive improved system parameters for the HD 209458 system using a model that simultaneously fits both photometric transit and radial velocity observations. The photometry consists of previous Hubble Space Telescope STIS and FGS observations, 12 I-band transits observed between 2001 and 2003 with the Mount Laguna Observatory 1 m telescope, and six Strömgren b + y transits observed between 2001 and 2004 with two of the Automatic Photometric Telescopes at Fairborn Observatory. The radial velocities were derived from Keck HIRES observations. The model properly treats the orbital dynamics of the system and thus yields robust and physically self-consistent solutions. Our set of system parameters agrees with previously published results, although with improved accuracy. For example, applying robust limits on the stellar mass of 0.93-1.20 M☉, we find 1.26RJ < Rplanet < 1.42RJ and 0.59MJ < Mplanet < 0.70MJ. We can reduce the uncertainty of these estimates by including a stellar mass-radius relation constraint, yielding Rplanet = RJ and Mplanet = MJ. Our results verify that the planetary radius is 10%-20% larger than predicted by irradiated planet evolution models, confirming the need for an additional mechanism to slow the evolutionary contraction of the planet. A revised ephemeris is derived, T0 = 2,452,854.82545 + 3.52474554E (HJD), which now contains an uncertainty in the period of 0.016 s and should facilitate future searches for planetary satellites and other bodies in the HD 209458 system.