Linear Isentropic Oscillations of Stars [recurso electrónico] : Theoretical Foundations / by Paul Smeyers, Tim Van Hoolst.

Por: Smeyers, Paul [author.]Colaborador(es): Van Hoolst, Tim [author.] | SpringerLink (Online service)Tipo de material: TextoTextoSeries Astrophysics and Space Science Library ; 371Editor: Berlin, Heidelberg : Springer Berlin Heidelberg : Imprint: Springer, 2010Descripción: XIV, 473 p. online resourceTipo de contenido: text Tipo de medio: computer Tipo de portador: online resourceISBN: 9783642130304Tema(s): Physics | Mechanics | Thermodynamics | Acoustics | Physics | Astrophysics and Astroparticles | Mechanics | Thermodynamics | AcousticsFormatos físicos adicionales: Printed edition:: Sin títuloClasificación CDD: 523.01 Clasificación LoC:QB460-466Recursos en línea: Libro electrónicoTexto
Contenidos:
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 Representation of 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.
En: Springer eBooksResumen: 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, the origin 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.
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Existencias
Tipo de ítem Biblioteca actual Colección Signatura Copia número Estado Fecha de vencimiento Código de barras
Libro Electrónico Biblioteca Electrónica
Colección de Libros Electrónicos QB460 -466 (Browse shelf(Abre debajo)) 1 No para préstamo 374393-2001

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 Representation of 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.

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, the origin 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.

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