HAT-P-7b: An Extremely Hot Massive Planet Transiting a Bright Star in the Kepler Field
HAT-P-7b: An Extremely Hot Massive Planet Transiting a Bright Star in the Kepler Field
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DOI：
10.1086/588010
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发表时间：
2008-03
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影响因子：
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通讯作者：
A. Pál;G. Bakos;G. Torres;R. W. Noyes;D. Latham;G. Kovacs;G. Marcy;D. Fischer;R. P. Butler;D. Sasselov;B. Sipocz;G. Esquerdo;G. Kovacs;R. Stefanik;J. Lázár;I. Papp;P. S. CfA;D. O. Astronomy;E. University;Nsf Fellow;K. Observatory;Uc Berkeley;D. Physics;Astronomy;San Diego State University;D. Magnetism;Carnegie Institution of Washington;Hungarian Astronomical Association
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文献类型：
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作者：
A. Pál;G. Bakos;G. Torres;R. W. Noyes;D. Latham;G. Kovacs;G. Marcy;D. Fischer;R. P. Butler;D. Sasselov;B. Sipocz;G. Esquerdo;G. Kovacs;R. Stefanik;J. Lázár;I. Papp;P. S. CfA;D. O. Astronomy;E. University;Nsf Fellow;K. Observatory;Uc Berkeley;D. Physics;Astronomy;San Diego State University;D. Magnetism;Carnegie Institution of Washington;Hungarian Astronomical Association
我们报道了HATNet项目的最新发现：一颗非常热的巨行星围绕一颗明亮的（V = 10.5）星星运行，其小半长轴为a = 0.0377 ± 0.0005 Au。系统星历P = 2.2047299 ± 0.0000040天，中天时间E = 2，453，790.2593 ± 0.0010（BJD）。根据主星星星的光谱数据和光度测量，这颗行星的质量为Mp = 1.78+ 0.08−0.05 MJ，半径为Rp = 1.36+ 0.20−0.09 RJ。母星星是一颗稍微演化的F6星星，M = 1.47+ 0.08−0.05 M，R = 1.84+ 0.23−0.11 R，Teff = 6350 ± 80 K，金属量[ Fe/H ] = + 0.26 ± 0.08。相对较热和较大的主星星，加上行星的近轨道，产生了非常高的行星辐照度4.71+ 1.44−0.05 × 109 erg cm−2 s−1，这使行星接近Fortney等人定义的pM类辐照行星的顶部。白天的温度应该是2730+ 150−100 K。由于主星星星非常明亮，地面望远镜测量二次日食应该是可行的，这为将当前热木星大气模型的预测与观测结果进行比较提供了一个很好的机会。此外，主星星福尔斯落在即将进行的开普勒使命的区域内;因此，将有可能进行广泛的空间后续行动，不仅包括主要的凌日和二次日食观测，而且还包括星震学。
We report on the latest discovery of the HATNet project: a very hot giant planet orbiting a bright (V = 10.5) star with a small semimajor axis of a = 0.0377 ± 0.0005 AU. Ephemeris for the system is P = 2.2047299 ± 0.0000040 days, midtransit time E = 2,453,790.2593 ± 0.0010 (BJD). Based on the available spectroscopic data on the host star and photometry of the system, the planet has a mass of Mp = 1.78+ 0.08−0.05 MJ and radius of Rp = 1.36+ 0.20−0.09 RJ. The parent star is a slightly evolved F6 star with M⋆ = 1.47+ 0.08−0.05 M☉, R⋆ = 1.84+ 0.23−0.11 R☉, Teff = 6350 ± 80 K, and metallicity [ Fe/H ] = + 0.26 ± 0.08. The relatively hot and large host star, combined with the close orbit of the planet, yield a very high planetary irradiance of 4.71+ 1.44−0.05 × 109 erg cm−2 s−1, which places the planet near the top of the pM class of irradiated planets as defined by Fortney et al. If as predicted by Fortney et al. the planet reradiates its absorbed energy before distributing it to the night side, the day-side temperature should be about 2730+ 150−100 K. Because the host star is quite bright, measurement of the secondary eclipse should be feasible for ground-based telescopes, providing a good opportunity to compare the predictions of current hot Jupiter atmospheric models with the observations. Moreover, the host star falls in the field of the upcoming Kepler mission; hence extensive space-borne follow-up, including not only primary transit and secondary eclipse observations but also asteroseismology, will be possible.