Asteroseismology and extrasolar planets of K giants

Computer Science

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Stars: Pulsations, K Giants, Planets: Exoplanets

Scientific paper

A decade ago precise radial velocity (RV) studies established that K giant stars were a new class of variable stars. This variability occurs on two time scales: 2-10 days and several hundreds of days. The short period variability is clearly due to p-mode oscillations. The best studied K giants (Arcturus and α UMa, using photometry) show up to 10 RV modes that are equally spaced in frequency, i.e. the characteristics of p-mode oscillations. The multi-mode nature of these pulsations make these objects ideal targets for asteroseismic studies with Eddington. The expected high photometric amplitude (a few mmag) and long time scales (days) means that these objects can be studied using the exoplanet field of Eddington. Asteroseismic studies of these stars can be used to derive such fundamental parameters as the stellar mass and radius as well as determine the internal structure of the star which can be compared to stellar evolution theory. The nature of many of the long period variations is uncertain and these may be due to nonradial pulsations, rotational modulation by surface features, or planetary companions. The recent discovery of planetary companions to several K giants lends some support to the companion hypothesis. Eddington can help establish the nature of the long period variations since pulsations or surface structure should be accompanied by photometric variations. Furthermore, asteroseismic studies of K giant using Eddington may establish the progenitor star and this can provide us with a sample of previous A-F main sequence stars for which can be surveyed for extrasolar planets.

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