HAT-P-65b AND HAT-P-66b: TWO TRANSITING INFLATED HOT JUPITERS AND OBSERVATIONAL EVIDENCE FOR THE REINFLATION OF CLOSE-IN GIANT PLANETS
HAT-P-65b AND HAT-P-66b: TWO TRANSITING INFLATED HOT JUPITERS AND OBSERVATIONAL EVIDENCE FOR THE REINFLATION OF CLOSE-IN GIANT PLANETS
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HAT-P-65b 和 HAT-P-66b：两颗凌日膨胀热木星以及近距离巨行星再膨胀的观测证据
DOI：
10.3847/0004-6256/152/6/182
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发表时间：
2016
期刊：
影响因子：
--
通讯作者：
P. S'ari
中科院分区：
文献类型：
--
作者：
J. Hartman;G. Bakos;W. Bhatti;K. Penev;A. Bieryla;D. Latham;G. Kov'acs;G. Torres;Z. Csubry;Miguel de Val;L. Buchhave;T. Kov'acs;S. Quinn;A. Howard;H. Isaacson;B. Fulton;M. Everett;G. Esquerdo;B. B'eky;T. Szklenár;E. Falco;A. Santerne;I. Boisse;G. H'ebrard;A. Burrows;J. L'az'ar;I. Papp;P. S'ari
我们目前发现的凌日系外行星HAT-P-65 b和HAT-P-66 b，轨道周期和天，质量和，膨胀半径和，分别。它们围绕着中等亮度的恒星运行。恒星在主序星的转折点。虽然众所周知，近距离巨行星的半径与它们的平衡温度相关，但行星的半径是否会随着它们的宿主进化而增加，变得更加明亮，这是一个悬而未决的问题。通过观察更广泛的近距离凌日巨行星样本，我们发现行星半径与其宿主恒星的分数年龄之间存在统计学显著相关性，误报概率仅为0.0041%。我们发现，行星半径和其宿主的分数年龄之间的相关性可以用行星半径和它们现在的平衡温度之间的已知相关性来充分解释;然而，如果用零年龄的主序平衡温度代替现在的平衡温度，那么还必须包括与年龄的相关性来解释行星半径。这表明，在主序前收缩后，由于从其宿主恒星接收到的辐射水平不断增加，近距离的巨行星会随着时间的推移而重新膨胀。先前的理论工作表明，这种对辐射的动态响应需要很大一部分入射能量沉积在行星内部深处。
We present the discovery of the transiting exoplanets HAT-P-65b and HAT-P-66b, with orbital periods of and days, masses of and , and inflated radii of and , respectively. They orbit moderately bright ( and ) stars of mass and . The stars are at the main-sequence turnoff. While it is well known that the radii of close-in giant planets are correlated with their equilibrium temperatures, whether or not the radii of planets increase in time as their hosts evolve and become more luminous is an open question. Looking at the broader sample of well-characterized close-in transiting giant planets, we find that there is a statistically significant correlation between planetary radii and the fractional ages of their host stars, with a false-alarm probability of only 0.0041%. We find that the correlation between the radii of planets and the fractional ages of their hosts is fully explained by the known correlation between planetary radii and their present-day equilibrium temperatures; however, if the zero-age main-sequence equilibrium temperature is used in place of the present-day equilibrium temperature, then a correlation with age must also be included to explain the planetary radii. This suggests that, after contracting during the pre-main-sequence, close-in giant planets are reinflated over time due to the increasing level of irradiation received from their host stars. Prior theoretical work indicates that such a dynamic response to irradiation requires a significant fraction of the incident energy to be deposited deep within the planetary interiors.
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