arXiv 0907.28182009-07-16astro-ph.SR

黄色和红色脉动变星中的随机过程

Stochastic Processes in Yellow and Red Pulsating Variables

David G. Turner, J. R. Percy, T. Colivas, Leonid N. Berdnikov, Mohamed Abdel-Sabour Abdel-Latif

备注：: Poster given at the "Stellar Pulsation: Challenges for Theory and Observation" conference in Santa Fe, New Mexico (2009)
DOI：: 10.1063/1.3246435

摘要：

脉动周期的随机变化在冷的脉动星中得到了很好的证实，特别是红巨星变星：Miras，A型和B型的半正则星，以及RV Tau变星。这样的效应也在少数造父变星、SX Phe变星XX Cyg，以及最近的红超巨星变星BC Cyg（一颗C型半正则变星）中观察到。这种波动的性质在恒星的几个脉动周期内似乎是随机的，但主要脉动机制的规律性在长期内占主导地位。随机性的程度与恒星的尺寸有关，随机性参数“e”似乎与周期“P”内的平均恒星半径密切相关，平均值为e/P = 0.0136+-0.0005。造成这种波动的物理过程是不确定的，但推测起源于此类恒星中包层对流的时间变化。

英文摘要：

Random changes in pulsation period are well established in cool pulsating stars, in particular the red giant variables: Miras, semi-regulars of types A and B, and RV Tau variables. Such effects are also observed in a handful of Cepheids, the SX Phe variable XX Cyg, and, most recently, the red supergiant variable, BC Cyg, a type C semi-regular. The nature of such fluctuations is seemingly random over a few pulsation cycles of the stars, yet the regularity of the primary pulsation mechanism dominates over the long term. The degree of stochasticity is linked to the dimensions of the stars, the randomness parameter 'e' appearing to correlate closely with mean stellar radius through the period 'P', with an average value of e/P = 0.0136+-0.0005. The physical processes responsible for such fluctuations are uncertain, but presumably originate in temporal modifications of envelope convection in such stars.

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英文摘要：

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