Abstract
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 1000 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.
Original language | English |
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Pages (from-to) | 542-550 |
Number of pages | 9 |
Journal | Royal Astronomical Society. Monthly Notices |
Volume | 408 |
Issue number | 1 |
DOIs | |
Publication status | Published - 11 Oct 2010 |
Keywords
- stars: oscillations
- methods: data analysis
- methods: statistical