On the pulsation of a star in which there is a prevalent magnetic field

Chandrasekhar, S. ; Nelson Limber, D. (1954) On the pulsation of a star in which there is a prevalent magnetic field Astrophysical Journal, 119 . pp. 10-13. ISSN 0004-637X

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Official URL: http://adsabs.harvard.edu/abs/1954ApJ...119...10C

Related URL: http://dx.doi.org/10.1086/145791

Abstract

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 σ2I = - (3γ - 4) (Ω + B) , where γ is the ratio of the specific heats, I = ∫0Mr2dm (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.

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ID Code:76771
Deposited On:07 Jan 2012 04:18
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