The effects of stellar population synthesis on the distributions of the asteroseismic observables ν_max and Δν of red-clump stars

Abstract

The distributions of the frequencies of the maximum oscillation Power (ν_max) and the large frequency separation ( Δν) of red giant stars observed by CoRoT have a dominant peak. Miglio et al. (2009) identified that the stars are red-clump stars. Using stellar population synthesis method, we studied the effects of Reimers mass loss, binary interactions, star formation rate and the mixing-length parameter on the distributions of the ν_max and Δν of red-clump stars. The Reimers mass loss can result in an increase in the ν_max and Δν of old population which lost a considerable amount of mass. However, it leads to a small decrease in those of middle-age population which lost a little bit of mass. Furthermore, a high mass-loss rate impedes the low-mass and low-metal stars evolving into core-helium burning (CHeB) stage. Both Reimers mass loss and star formation rate mainly affect the number of CHeB stars with ν_max and Δν, but hardly affect the peak locations of ν_max and Δν. Binary interactions also can lead to an increase or decrease in the ν_max and Δν of some stars. However, the fraction of CHeB stars undergoing binary interactions is very small in our simulations. Therefore, the peak locations are also not affected by binary interactions. The non-uniform distributions of ν_max and Δν are mainly caused by the most of red-clump stars having an approximate radius rather than mass. The radius of red-clump stars decreases with increasing the mixing-length parameter. The peak locations of ν_max and Δν can, thus, be affected by the mixing-length parameter.

7 pages, 9 figures; accepted for publication in MNRAS

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