Research Papers in Physics and Astronomy

 

Date of this Version

4-1979

Document Type

Article

Citation

The Astrophysical Journal, Vol. 156, April 1969

Comments

Copyright 1969. The University of Chicago. All rights reserved.

Abstract

This Note will present briefly some general properties of nuclear-energized pulsations of stars as treated in the linear quasi-adiabatic theory. In particular, the results will be derived from a number of detailed calculations of stellar models.

It is well known that an upper limit for the fundamental eigenfrequency of radial pulsation Ѡ0 is given by

Ѡmax2 = 1ʃ0(3Γ1 ‒ 4)q/x dq / 1ʃ0 x2dq,

Ѡ2= (2∏/Period)2 R3/GM

(e.g., Ledoux and Walraven 1958). According to this expression, Ѡmax2 increases both with decreasing radiation pressure (i.e., increasing Γ1) and with increasing central condensation as measured by the ratio of integrals

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