KEPLER-21b: A 1.6 REarth PLANET TRANSITING THE BRIGHT OSCILLATING F SUBGIANT STAR HD 179070
KEPLER-21b: A 1.6 REarth PLANET TRANSITING THE BRIGHT OSCILLATING F SUBGIANT STAR HD 179070
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KEPLER-21b：一颗 1.6 地球行星凌日明亮振荡 F 次巨星 HD 179070
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发表时间：
2011
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通讯作者：
C. Henze
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作者：
S. Howell;J. Rowe;S. Bryson;S. Quinn;G. Marcy;H. Isaacson;D. Ciardi;W. Chaplin;T. Metcalfe;M. Monteiro;T. Appourchaux;S. Basu;O. Creevey;R. Gilliland;P. Quirion;D. Stello;H. Kjeldsen;J. Christensen;Y. Elsworth;Rafael A. Garc'ia;G. Houdek;C. Karoff;J. Molenda–Żakowicz;M. Thompson;G. Verner;G. Torres;F. Fressin;J. Crepp;E. Adams;A. Dupree;D. Sasselov;C. Dressing;W. Borucki;D. Koch;J. Lissauer;D. Latham;L. Buchhave;T. Gautier;M. Everett;E. Horch;N. Batalha;E. Dunham;P. Szkody;D. R. Silva;K. Mighell;J. Holberg;J. Ballot;T. Bedding;H. Bruntt;T. Campante;R. Handberg;S. Hekker;D. Huber;S. Mathur;B. Mosser;C. R'egulo;T. White;J. Christiansen;C. Middour;M. Haas;J. Hall;J. Jenkins;Sean McCaulif;M. Fanelli;C. Kulesa;D. Mccarthy;C. Henze
我们提出开普勒观测明亮（V = 8.3），振荡的星星HD 179070。观测显示出类似凌日的事件，揭示了一个1.6 REarth的小天体每2.8天绕星星一周。利用开普勒短节奏观测对HD 179070进行的地震研究表明，HD 179070的频率功率谱与类似太阳的声波p模式振荡一致。天文地震分析提供了HD 179070的质量和半径分别为1.34 ± 0.06 M和1.86 ± 0.04 R，以及这个F5亚巨星的年龄为2.84 ± 0.34 Gyr。结合地面跟踪观测、开普勒光变曲线和图像数据分析以及混合情景模型，我们保守地表明，在>99.7%的置信水平（3σ）下，凌日事件是由一颗1.64 ± 0.04地球日的系外行星在2.785755 ± 0.000032天的轨道上引起的。这颗系外行星距离星星只有0.04 Au，我们的光谱观测提供了它的质量上限为1000万（2σ）。HD 179070是开普勒发现的最亮的系外行星宿主星星。
We present Kepler observations of the bright (V = 8.3), oscillating star HD 179070. The observations show transit-like events which reveal that the star is orbited every 2.8 days by a small, 1.6 REarth object. Seismic studies of HD 179070 using short cadence Kepler observations show that HD 179070 has a frequency–power spectrum consistent with solar-like oscillations that are acoustic p-modes. Asteroseismic analysis provides robust values for the mass and radius of HD 179070, 1.34 ± 0.06 M☉ and 1.86 ± 0.04 R☉, respectively, as well as yielding an age of 2.84 ± 0.34 Gyr for this F5 subgiant. Together with ground-based follow-up observations, analysis of the Kepler light curves and image data, and blend scenario models, we conservatively show at the >99.7% confidence level (3σ) that the transit event is caused by a 1.64 ± 0.04 REarth exoplanet in a 2.785755 ± 0.000032 day orbit. The exoplanet is only 0.04 AU away from the star and our spectroscopic observations provide an upper limit to its mass of ∼10 MEarth (2σ). HD 179070 is the brightest exoplanet host star yet discovered by Kepler.