Date of this Version
The Astrophysical Journal, Vol. 156, April 1969
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