Asteroseismology of solar-type stars: signatures of convective and/or helium cores

被引：13

作者：

Soriano, M. ^{[1
]}

Vauclair, S. ^{[1
]}

机构：

[1] Univ Toulouse, CNRS, Lab Astrophys Toulouse Tarbes, UMR 5572, F-31400 Toulouse, France

来源：

ASTRONOMY & ASTROPHYSICS | 2008年 / 488卷 / 03期

关键词：

stars : oscillations; stars : abundances; stars : evolution; stars : planetary systems; galaxy : kinematics and dynamics; galaxy : open clusters and associations : general;

D O I：

10.1051/0004-6361:200809977

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Aims. Several frequency combinations are widely used in the analysis of stellar oscillations for comparisons between models and observations. In particular, the "small separations" can help constraining the stellar cores. We showed in a previous paper that they can change sign, in contradiction with the "asymptotic theory", and that this behaviour could correspond to signatures of convective and/or helium cores. Here we analyse this behaviour in detail by systematic modelling during stellar evolution. Methods. We computed evolutionary tracks for models with various masses (from 1.05 to 1.25 M-circle dot) and various chemical compositions, with and without overshooting. We computed the adiabatic oscillation frequencies of the models and analysed the evolution of their small separations along an evolutionary track. Results. We find that, for all cases, the stars go through a stage during their evolution, where the small separations computed between degrees l = 0 and l = 2 become negative in the observed range of frequencies. This behaviour is clearly related to the signature of a helium-rich core. We discuss the consequences for interpreting of the acoustic frequencies observed in solar-type stars.

引用

页码：975 / 985

页数：11

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