湍动对流与变星脉动稳定性
发布时间：2019-05-20 04:36
【摘要】：对低温变星的脉动激发机制中的一些争议问题进行了评述:(1)大多数人相信γDoradus型变星是由所谓的阻塞对流机制所激发.研究表明,γDoradus和δScuti变星的激发机制不存在任何实质性的差别,他们是更大一类δScuti-γDoradus变星的2个次群:δScuti变星是p模脉动子群;而γDoradus是g模脉动子群.(2)大多数人相信太阳5分钟振荡和恒星的类太阳振荡被对流所阻尼,他们是由所谓湍流随机激发机制驱动的.研究表明,对流并非单纯只是脉动的阻尼机制,否则无法解释Mira变星和类Mira变星.利用非局部和非定常的恒星对流理论,不仅可以重现δScuti和γDoradus脉动不稳定区,也可重现低光度红巨星的类太阳振荡和高光度红巨星的类Mira振荡特性.
[Abstract]:In this paper, some controversial issues in the pulsating excitation mechanism of low temperature variable stars are reviewed: (1) most people believe that the gamma Doradus variable star is excited by the so-called blocking convective mechanism. It is shown that there is no substantial difference in the excitation mechanism between 纬 Doradus and 未 Scuti variable stars. They are two order groups of a larger class of 未 Scuti- 纬 Doradus variable stars: 未 Scuti variable stars are p mode pulsating subgroup; Gamma Doradus is a g-mode pulsating subgroup. (2) most people believe that the solar 5-minute oscillations and the solar-like oscillations of stars are damped by convection, which are driven by the so-called turbulent random excitation mechanism. The results show that the convection is not just the damping mechanism of pulsation, otherwise it can not explain the Mira variable star and the Mira-like variable star. By using the nonlocal and unstable stellar convective theory, not only the fluctuating unstable regions of 未 Scuti and gamma Doradus can be reproduced, but also the solar-like oscillations of low-luminance red superstars and the Mira-like oscillations of high-luminance red superstars can be reproduced.
【作者单位】： 中国科学院紫金山天文台;
【基金】：国家自然科学基金项目(AO11373069)资助
【分类号】：P145.2
本文编号：2481354
[Abstract]:In this paper, some controversial issues in the pulsating excitation mechanism of low temperature variable stars are reviewed: (1) most people believe that the gamma Doradus variable star is excited by the so-called blocking convective mechanism. It is shown that there is no substantial difference in the excitation mechanism between 纬 Doradus and 未 Scuti variable stars. They are two order groups of a larger class of 未 Scuti- 纬 Doradus variable stars: 未 Scuti variable stars are p mode pulsating subgroup; Gamma Doradus is a g-mode pulsating subgroup. (2) most people believe that the solar 5-minute oscillations and the solar-like oscillations of stars are damped by convection, which are driven by the so-called turbulent random excitation mechanism. The results show that the convection is not just the damping mechanism of pulsation, otherwise it can not explain the Mira variable star and the Mira-like variable star. By using the nonlocal and unstable stellar convective theory, not only the fluctuating unstable regions of 未 Scuti and gamma Doradus can be reproduced, but also the solar-like oscillations of low-luminance red superstars and the Mira-like oscillations of high-luminance red superstars can be reproduced.
【作者单位】： 中国科学院紫金山天文台;
【基金】：国家自然科学基金项目(AO11373069)资助
【分类号】：P145.2
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