太阳型振荡器功率谱自协方差模型
Modelling the Autocovariance of the Power Spectrum of a Solar-Type Oscillator
摘要：
天文地震学能够通过分析恒星声谱来对太阳型恒星的内部进行研究。然而，这样的分析过程往往不得不依赖于整个过程中做出的主观选择。一个反复出现的问题是确定声谱中的信号是源自径向振荡模式还是偶极振荡模式。为了克服这个问题，我们提出了一个程序的建模和拟合的自协方差的功率谱，可用于获得全球地震参数的太阳型恒星，这样做的自动化的方式，而不需要作出主观的选择。从一组可检索的全球地震参数，我们强调的平均小频率分离，并根据功率谱的固有特性，平均旋转频率分裂。由于这一过程是自动化的，它可以作为一个有用的工具，在分析一千多个太阳型恒星预计将被观察到的开普勒天文地震调查（KAI）的一部分。我们将上述过程应用于太阳的模拟。假设不同的视星等，我们解决的问题，如何准确地和如何精确地，我们可以检索的几个全球地震参数的太阳被观察到的KAI的一部分。
英文摘要：
Asteroseismology is able to conduct studies on the interiors of solar-type stars from the analysis of stellar acoustic spectra. However, such an analysis process often has to rely upon subjective choices made throughout. A recurring problem is to determine whether a signal in the acoustic spectrum originates from a radial or a dipolar oscillation mode. In order to overcome this problem, we present a procedure for modelling and fitting the autocovariance of the power spectrum which can be used to obtain global seismic parameters of solar-type stars, doing so in an automated fashion without the need to make subjective choices. From the set of retrievable global seismic parameters we emphasize the mean small frequency separation and, depending on the intrinsic characteristics of the power spectrum, the mean rotational frequency splitting. Since this procedure is automated, it can serve as a useful tool in the analysis of the more than one thousand solar-type stars expected to be observed as part of the Kepler Asteroseismic Investigation (KAI). We apply the aforementioned procedure to simulations of the Sun. Assuming different apparent magnitudes, we address the issues of how accurately and how precisely we can retrieve the several global seismic parameters were the Sun to be observed as part of the KAI.
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