SOLAR-LIKE OSCILLATIONS IN KIC 11395018 AND KIC 11234888 FROM 8 MONTHS OF KEPLER DATA
SOLAR-LIKE OSCILLATIONS IN KIC 11395018 AND KIC 11234888 FROM 8 MONTHS OF KEPLER DATA
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DOI：
10.1088/0004-637x/733/2/95
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发表时间：
2011-03
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通讯作者：
S. Mathur;R. Handberg;T. Campante;R. García;T. Appourchaux;T. Bedding;B. Mosser;W. Chaplin;J. Ballot;O. Benomar;A. Bonanno;E. Corsaro;P. Gaulme;S. Hekker;C. Régulo;D. Salabert;G. Verner;T. White;I. Brandao;O. Creevey;G. Doğan;Y. Elsworth;D. Huber;S. Hale;G. Houdek;C. Karoff;T. Metcalfe;J. Molenda–Żakowicz;M. Monteiro;Michael Thompson;J. Christensen-Dalsgaard;R. Gilliland;S. Kawaler;H. Kjeldsen;E. Quintana;D. Sanderfer;S. Seader
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作者：
S. Mathur;R. Handberg;T. Campante;R. García;T. Appourchaux;T. Bedding;B. Mosser;W. Chaplin;J. Ballot;O. Benomar;A. Bonanno;E. Corsaro;P. Gaulme;S. Hekker;C. Régulo;D. Salabert;G. Verner;T. White;I. Brandao;O. Creevey;G. Doğan;Y. Elsworth;D. Huber;S. Hale;G. Houdek;C. Karoff;T. Metcalfe;J. Molenda–Żakowicz;M. Monteiro;Michael Thompson;J. Christensen-Dalsgaard;R. Gilliland;S. Kawaler;H. Kjeldsen;E. Quintana;D. Sanderfer;S. Seader
我们分析了开普勒使命在前8个月的观测两个太阳型恒星的光谱类型G和F：KIC 11395018和KIC 11234888，分别获得的测光短节奏的数据，后者具有较低的信号噪声比（S/N）相比，前者。我们估计全局参数的声学（p）模式，如平均大小的频率分离，最大的p模式包络的频率，和平均线宽的声学模式。我们能够识别和测量的第一个星星和第二个16，即使这些恒星的S/N是相当低的22 p-模式频率。我们还从功率谱密度的低频部分的分析中得到了一些关于恒星自转周期的信息。一个独立于模型的平均密度，质量和半径的估计得到使用的标度律。我们强调的重要性，持续观测的恒星与低S/N的振荡模式的改进表征。我们的研究结果提供了一个预览什么将是可能的许多恒星与长期的数据集在剩余的使命。
We analyze the photometric short-cadence data obtained with the Kepler mission during the first 8 months of observations of two solar-type stars of spectral types G and F: KIC 11395018 and KIC 11234888, respectively, the latter having a lower signal-to-noise ratio (S/N) compared with the former. We estimate global parameters of the acoustic (p) modes such as the average large and small frequency separations, the frequency of the maximum of the p-mode envelope, and the average line width of the acoustic modes. We were able to identify and to measure 22 p-mode frequencies for the first star and 16 for the second one even though the S/N of these stars are rather low. We also derive some information about the stellar rotation periods from the analyses of the low-frequency parts of the power spectral densities. A model-independent estimation of the mean density, mass, and radius is obtained using the scaling laws. We emphasize the importance of continued observations for the stars with low S/N for an improved characterization of the oscillation modes. Our results offer a preview of what will be possible for many stars with the long data sets obtained during the remainder of the mission.