THE TREATMENT OF HIGHLY NONADIABATIC, NONRADIAL PULSATIONS BY APPLICATION OF THE RICCATI METHOD TO THE EXAMPLE OF HYDROGEN-DEFICIENT CARBON STARS

被引:27
作者
GLATZEL, W [1 ]
GAUTSCHY, A [1 ]
机构
[1] MAX PLANCK INST PHYS & ASTROPHYS,INST ASTROPHYS,W-8046 GARCHING,GERMANY
关键词
INSTABILITIES; STARS; CARBON; INTERIORS; OSCILLATIONS;
D O I
10.1093/mnras/256.2.209
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
The Riccati method, developed to solve the linear boundary-value problem of radial stellar pulsations, is generalized and shown to be applicable to the calculation of non-radial, non-adiabatic oscillations. Its advantages are demonstrated for the extreme example of a highly non-adiabatic helium star. The acoustic spectrum of helium stars is studied in detail. Mode-coupling instabilities occur in the non-radial spectrum for a wide range of the harmonic degree l, their appearance being similar to the radial case studied previously. With increasing l, the width of the instability strip in the HRD - extending up to log T(eff) almost-equal-to 4.3 for low l - shrinks and the growth rates of the instabilities decrease. Stabilization is reached between l = 10 and 100.
引用
收藏
页码:209 / 218
页数:10
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