Linear Isentropic Oscillations of Stars

The study of stellar oscillations is the preeminent way to investigate the stability of stars and to interpret their variability. The theory of the linear, isentropic oscillations of isolated gaseous stars, and thus of compressible spherically symmetric equilibrium configurations, has largely been developed from the viewpoint of the hypothesis of the physical radial pulsations of stars. Written for doctoral students and researchers, this monograph aims to provide a systematic and consistent survey of the fundamentals of the theory of free, linear, isentropic oscillations in spherically symmetric, gaseous equilibrium stars. The first part of the book presents basic concepts and equations, the distinction between spheroidal and toroidal normal modes, the solution of Poisson's differential equation for the perturbation of the gravitational potential, and Hamilton's variational principle. The second part is devoted to the possible existence of waves propagating in the radial direction, theorigin and classification of normal modes, the completeness of the normal modes, and the relation between the local stability with respect to convection and the global stability of a star. The third part deals with asymptotic representations of normal modes and with slow period changes in rapidly evolving pulsating stars.

Provides a comprehensive presentation of the fundamental aspects of the theory of the linear, isentropic oscillations in spherically symmetric stars Intermediate steps in the mathematical derivations included With extensive appendices on fundamental mathematical and theoretical physics problems Includes supplementary material: sn.pub/extras

Auteur

Paul Smeyers is professor em. in astrophysics at the Institute of Astronomy of the Catholic University Leuven, Belgium. Tim Van Hoolst is part-time professor at the same institute and senior research scientist at the Royal Observatory of Belgium. Both are long-time teachers and researcers in the field of stellar oscillations.

Résumé

This book surveys the theory of free, linear, isentropic oscillations in spherically symmetric, gaseous equilibrium stars, from basic concepts to asymptotic representations of normal modes and with slow period changes in rapidly evolving pulsating stars.

Contenu
Basic Concepts.- The Equations Governing Linear Perturbations in a Quasi-Static Star.- Deviations from the Hydrostatic and Thermal Equilibrium in a Quasi-Static Star.- Eigenvalue Problem of the Linear, Isentropic Normal Modes in a Quasi-Static Star.- Spheroidal and Toroidal Normal Modes.- Determination of Spheroidal Normal Modes: Mathematical Aspects.- The Eulerian Perturbation of the Gravitational Potential.- The Variational Principle of Hamilton.- Radial Propagation of Waves.- Classification of the Spheroidal Normal Modes.- Classification of the Spheroidal Normal Modes (continued).- Completeness of the Linear, Isentropic Normal Modes.- N 2(r) Nowhere Negative as Condition for Non-Radial Modes with Real Eigenfrequencies.- Asymptotic Representation of Low-Degree, Higher-Order p-Modes.- Asymptotic Representation of Low-Degree and Intermediate-Degree p-Modes.- Asymptotic Representation of Low-Degree, Higher-Order g +-Modes in Stars Containing a Convective Core.- Asymptotic Representationof Low-Degree, Higher-Order g +-Modes in Stars Consisting of a Radiative Core and a Convective Envelope.- High-Degree, Low-Order Modes.- Period Changes in a Rapidly Evolving Pulsating Star.