A UNIFORM ASTEROSEISMIC ANALYSIS OF 22 SOLAR-TYPE STARS OBSERVED BY KEPLER
A UNIFORM ASTEROSEISMIC ANALYSIS OF 22 SOLAR-TYPE STARS OBSERVED BY KEPLER
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DOI：
10.1088/0004-637x/749/2/152
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发表时间：
2012-02
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通讯作者：
S. Mathur;T. Metcalfe;M. Woitaszek;H. Bruntt;G. Verner;J. Christensen-Dalsgaard;J. Christensen-Dalsgaard;O. Creevey;G. Doğan;G. Doğan;S. Basu;C. Karoff;C. Karoff;D. Stello;T. Appourchaux;T. Campante;T. Campante;W. Chaplin;R. García;T. Bedding;O. Benomar;A. Bonanno;S. Deheuvels;Y. Elsworth;P. Gaulme;J. Guzik;R. Handberg;S. Hekker;S. Hekker;W. Herzberg;M. Monteiro;L. Piau;P. Quirion;C. Régulo;C. Régulo;M. Roth;D. Salabert;A. Serenelli;Michael Thompson;R. Trampedach;T. White;J. Ballot;I. Brandao;J. Molenda–Żakowicz;H. Kjeldsen;J. Twicken;K. Uddin;B. Wohler
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作者：
S. Mathur;T. Metcalfe;M. Woitaszek;H. Bruntt;G. Verner;J. Christensen-Dalsgaard;J. Christensen-Dalsgaard;O. Creevey;G. Doğan;G. Doğan;S. Basu;C. Karoff;C. Karoff;D. Stello;T. Appourchaux;T. Campante;T. Campante;W. Chaplin;R. García;T. Bedding;O. Benomar;A. Bonanno;S. Deheuvels;Y. Elsworth;P. Gaulme;J. Guzik;R. Handberg;S. Hekker;S. Hekker;W. Herzberg;M. Monteiro;L. Piau;P. Quirion;C. Régulo;C. Régulo;M. Roth;D. Salabert;A. Serenelli;Michael Thompson;R. Trampedach;T. White;J. Ballot;I. Brandao;J. Molenda–Żakowicz;H. Kjeldsen;J. Twicken;K. Uddin;B. Wohler
利用开普勒空间望远镜进行的星震学不仅提供了更好的系外行星及其宿主恒星的特征描述，而且还提供了一个新的窗口，可以了解该领域大量太阳型恒星的恒星结构和演化。我们进行了统一的分析，22个最明亮的asteroseisic目标的最高信噪比观察1个月，每个在第一年的使命，我们量化的精度和相对精度的asteroseisic恒星半径，质量和年龄的测定，可能使用各种方法。我们提出的每个星星的属性来自自动分析的个人振荡频率和其他观测约束使用Asteroseismic建模门户网站（AMP）的样本，我们比较它们的结果模型网格为基础的方法，适合全球振荡特性。我们发现，拟合单个频率通常会产生小行星地震半径和质量的精度为10.1%，年龄为2.5%的精度（分别比拟合全球振荡特性好2倍，5倍和8倍）。来自不同方法的结果之间的绝对一致性水平也是令人鼓舞的，基于模型网格的方法产生的半径和质量的估计值略小，相对于AMP，它为每个星星计算了大量的专用模型。随着在使命的剩余时间内获得更长的数据集，可能进行这类分析的目标样本将会增加。
Asteroseismology with the Kepler space telescope is providing not only an improved characterization of exoplanets and their host stars, but also a new window on stellar structure and evolution for the large sample of solar-type stars in the field. We perform a uniform analysis of 22 of the brightest asteroseismic targets with the highest signal-to-noise ratio observed for 1 month each during the first year of the mission, and we quantify the precision and relative accuracy of asteroseismic determinations of the stellar radius, mass, and age that are possible using various methods. We present the properties of each star in the sample derived from an automated analysis of the individual oscillation frequencies and other observational constraints using the Asteroseismic Modeling Portal (AMP), and we compare them to the results of model-grid-based methods that fit the global oscillation properties. We find that fitting the individual frequencies typically yields asteroseismic radii and masses to ∼1% precision, and ages to ∼2.5% precision (respectively, 2, 5, and 8 times better than fitting the global oscillation properties). The absolute level of agreement between the results from different approaches is also encouraging, with model-grid-based methods yielding slightly smaller estimates of the radius and mass and slightly older values for the stellar age relative to AMP, which computes a large number of dedicated models for each star. The sample of targets for which this type of analysis is possible will grow as longer data sets are obtained during the remainder of the mission.