On the pulsation of a star in which there is a prevalent magnetic field
On the pulsation of a star in which there is a prevalent magnetic field
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关于存在普遍磁场的恒星的脉动
DOI：
10.1086/145791
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发表时间：
1954
期刊：
影响因子：
--
通讯作者：
D. N. Limber
中科院分区：
文献类型：
--
作者：
S. Chandrasekhar;D. N. Limber
本文给出了存在盛行磁场的气态恒星径向脉动频率（σ）的简单近似公式。公式为 σ 2 I = - (3γ - 4) (Ω + B) ，其中 γ 为比热容之比，I = ∫ 0 M r 2 dm (r) ，Ω 和 B 分别表示恒星的引力势能和磁能。该公式源自钱德拉塞卡和费米最近建立的维里定理；这也支持了他们的结论：只要使磁能接近维里定理所设定的上限（即|Ω|），就可以使脉动周期变得任意长。
In this paper a simple approximate formula is obtained for the frequency (σ) of radial pulsation of a gaseous star in which there is a prevalent magnetic field. The formula is σ 2 I = - (3γ - 4) (Ω + B) , where γ is the ratio of the specific heats, I = ∫ 0 M r 2 dm (r) , and Ω and B denote the gravitational potential energy and the magnetic energy of the star, respectively. The formula is derived from the virial theorem in the form recently established by Chandrasekhar and Fermi; and it supports their conclusion that the period of pulsation can be made as long as one may desire by letting the magnetic energy approach the upper limit (namely, |Ω|) set by the virial theorem.