湍動對流與變星脈動穩(wěn)定性
發(fā)布時間：2019-05-20 04:36
【摘要】：對低溫變星的脈動激發(fā)機制中的一些爭議問題進行了評述:(1)大多數(shù)人相信γDoradus型變星是由所謂的阻塞對流機制所激發(fā).研究表明,γDoradus和δScuti變星的激發(fā)機制不存在任何實質(zhì)性的差別,他們是更大一類δScuti-γDoradus變星的2個次群:δScuti變星是p模脈動子群;而γDoradus是g模脈動子群.(2)大多數(shù)人相信太陽5分鐘振蕩和恒星的類太陽振蕩被對流所阻尼,他們是由所謂湍流隨機激發(fā)機制驅(qū)動的.研究表明,對流并非單純只是脈動的阻尼機制,否則無法解釋Mira變星和類Mira變星.利用非局部和非定常的恒星對流理論,不僅可以重現(xiàn)δScuti和γDoradus脈動不穩(wěn)定區(qū),也可重現(xiàn)低光度紅巨星的類太陽振蕩和高光度紅巨星的類Mira振蕩特性.
[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 緯 Doradus and 未 Scuti variable stars. They are two order groups of a larger class of 未 Scuti- 緯 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.
【作者單位】： 中國科學(xué)院紫金山天文臺;
【基金】：國家自然科學(xué)基金項目(AO11373069)資助
【分類號】：P145.2
本文編號：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 緯 Doradus and 未 Scuti variable stars. They are two order groups of a larger class of 未 Scuti- 緯 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.
【作者單位】： 中國科學(xué)院紫金山天文臺;
【基金】：國家自然科學(xué)基金項目(AO11373069)資助
【分類號】：P145.2
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