Seismic modelling of the rotating, slowly pulsating B-type star HD 21071

被引：8
作者：
Szewczuk, W. [1 ]
Daszynska-Daszkiewicz, J. [1 ]
机构：
[1] Univ Wroclaw, Inst Astron, PL-51622 Wroclaw, Poland
来源：
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY | 2015年 / 453卷 / 01期
关键词：
stars: early-type; stars: oscillations; stars: rotation; LINE-PROFILE VARIATIONS; FREQUENCY NONRADIAL OSCILLATIONS; G-MODES; NONADIABATIC OBSERVABLES; IDENTIFICATION; INSTABILITY; VARIABLES; LIGHT;
D O I：
10.1093/mnras/stv1589
中图分类号：
P1 [天文学];
学科分类号：
0704 ;
摘要：
Interpretation of the oscillation spectrum of the slowly pulsating B-type (SPB) star HD 21071 is presented. We show that non-rotating models cannot account for the two highest amplitude frequencies and taking into account the effects of rotation is necessary. Rotating seismic models are constructed using various chemical compositions, opacity data, core overshooting parameters and rotational velocities. There are prospects for seismic modelling of SPB stars, even if no asymptotic pattern is observed in their oscillation spectra, provided an unambiguous mode identification is doable and the effects of rotation are properly included.
引用
收藏
页码：277 / 286
页数：10
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