Testing the asymptotic relation for period spacings from mixed modes of red giants observed with the Kepler mission
Testing the asymptotic relation for period spacings from mixed modes of red giants observed with the Kepler mission
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测试开普勒任务观测到的红巨星混合模式的周期间隔渐近关系
DOI：
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发表时间：
2016
期刊：
影响因子：
--
通讯作者：
P. Degroote
中科院分区：
文献类型：
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作者：
B. Buysschaert;B. Buysschaert;B. Buysschaert;P. Beck;P. Beck;E. Corsaro;J. Christensen;C. Aerts;C. Aerts;T. Arentoft;H. Kjeldsen;H. Kjeldsen;Rafael A. García;V. S. Aguirre;P. Degroote
美国宇航局开普勒太空望远镜在数千颗低质量红巨星上发现了连续径向顺序的偶极子混合脉动模式。这样的模式有可能揭示恒星内部深处的物理信息。人们提出了不同的方法来推导重力模周期间隔的观测值，其中最突出的方法依赖于应用于混合模的重力模特性的渐近脉动理论推导出的关系。我们的目的是比较基于这种渐近关系的结果与由经验方法得出的关于三颗脉动红巨星的结果。我们开发了一种数据驱动的方法来进行频率提取和模式识别。其次，利用已识别的偶极子混合模，利用经验方法和渐近关系确定重力场模周期间隔。在我们的方法中，我们考虑渐近关系的相位偏移$epsilon_{mathm {g}}$作为一个自由参数。利用样本中每颗恒星识别出的偶极子混合模式的频率，我们用两种不同的方法推导出了重力模式周期间隔的值。它们相差不到5%。由渐近关系推导的周期间隔平均精度优于1%，而数据驱动方法的平均精度为3%。由渐近关系得到的周期间隔值与由经验方法得到的周期间隔值很好地吻合。
Dipole mixed pulsation modes of consecutive radial order have been detected for thousands of low-mass red-giant stars with the NASA space telescope Kepler. Such modes have the potential to reveal information on the physics of the deep stellar interior. Different methods have been proposed to derive an observed value for the gravity-mode period spacing, the most prominent one relying on a relation derived from asymptotic pulsation theory applied to the gravity-mode character of the mixed modes. Our aim is to compare results based on this asymptotic relation with those derived from an empirical approach for three pulsating red-giant stars. We developed a data-driven method to perform frequency extraction and mode identification. Next, we used the identified dipole mixed modes to determine the gravity-mode period spacing by means of an empirical method and by means of the asymptotic relation. In our methodology, we consider the phase offset, $epsilon_{mathrm{g}}$, of the asymptotic relation as a free parameter. Using the frequencies of the identified dipole mixed modes for each star in the sample, we derived a value for the gravity-mode period spacing using the two different methods. These differ by less than 5%. The average precision we achieved for the period spacing derived from the asymptotic relation is better than 1%, while that of our data-driven approach is 3%. Good agreement is found between values for the period spacing derived from the asymptotic relation and from the empirical method.
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影响因子：
6.5
作者：
T. Kallinger;J. Ridder;S. Hekker;S. Mathur;S. Mathur;B. Mosser;M. Gruberbauer;M. Gruberbauer;R. García;C. Karoff;J. Ballot;J. Ballot
通讯作者：
T. Kallinger;J. Ridder;S. Hekker;S. Mathur;S. Mathur;B. Mosser;M. Gruberbauer;M. Gruberbauer;R. García;C. Karoff;J. Ballot;J. Ballot
六颗开普勒亚巨星和年轻红巨星内自转剖面径向依赖性的地震约束
影响因子：
6.5
作者：
Deheuvels;Doğan;Goupil
通讯作者：
Goupil