Abstract
The functions P0(m), r0(m), and ϱ0(m) are supposed to belong to a solution of the stellar-structure equations (9.1–4) for the case of complete equilibrium. Let us assume that we perturb the hydrostatic equilibrium, say by compressing the star slightly and releasing it again suddenly. It will expand and owing to inertia overshoot the equilibrium state: the star starts to oscillate. The analogy to the oscillating piston model (see §6.6) is obvious. More precisely we assume the initial displacement of the mass elements to be only radially directed (dϑ = dϕ = 0) and of constant absolute value on concentric spheres. This leads to purely radial oscillations (or radial pulsations) during which the star remains spherically symmetric all time. For the perturbed variables at time t we write
where the subscript 1 indicates the perturbations for which we have made a separation ansatz with an exponential time dependence [as in (25.17)]. The relative perturbations p, x, d are assumed to be ≪ 1.
Access this chapter
Tax calculation will be finalised at checkout
Purchases are for personal use only
Preview
Unable to display preview. Download preview PDF.
Author information
Authors and Affiliations
Rights and permissions
Copyright information
© 1990 Springer-Verlag Berlin Heidelberg
About this chapter
Cite this chapter
Kippenhahn, R., Weigert, A. (1990). Adiabatic Spherical Pulsations. In: Stellar Structure and Evolution. Astronomy and Astrophysics Library. Springer, Berlin, Heidelberg. https://doi.org/10.1007/978-3-642-61523-8_38
Download citation
DOI: https://doi.org/10.1007/978-3-642-61523-8_38
Publisher Name: Springer, Berlin, Heidelberg
Print ISBN: 978-3-540-58013-3
Online ISBN: 978-3-642-61523-8
eBook Packages: Springer Book Archive