Linear Isentropic Oscillations of Stars Theoretical Foundations
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 d...
| Main Authors: | , |
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| Format: | eBook |
| Language: | English |
| Published: |
Berlin, Heidelberg
Springer Berlin Heidelberg
2010, 2010
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| Edition: | 1st ed. 2010 |
| Series: | Astrophysics and Space Science Library
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| Subjects: | |
| Online Access: | |
| Collection: | Springer eBooks 2005- - Collection details see MPG.ReNa |
Table of Contents:
- 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