Relativistic stellar pulsations

Thesis/Dissertation · Thu Jan 01 04:00:00 EST 1987

OSTI ID:6967651

Finn, L S

A new formalism for the numerical study of g-modes in neutron stars is developed. This formalism avoids pitfalls associated with previous formalisms when applied to the study of these low-frequency modes. The formalism involves a new choice of perturbation variables, the introduction of an instantaneous gravity approximation to the field outside the star, and an energy principle for determining gravitational radiation damping times. The relativistic Cowling approximation, analogous to the Newtonian Cowling approximation, is refined to make it more accurate in the regime of highly relativistic stars. The approximation is used to prove a host of useful theorems regarding the non-radial modes of relativistic stars. Realistic neutron stars have a solid crust, and this will seriously affect their g-modes. The first steps toward developing a theory of nonradial relativistic pulsations in stars with a solid crust is reported on here. Solar five-minute oscillations are a weak source of gravitational radiation. The inner part of the solar system is actually in the transition zone of the solar-oscillation gravitational field, and future space-based beam detectors might be able to measure the solar transition-zone radiation.

• Research Organization: California Inst. of Tech., Pasadena (USA)
• OSTI ID: 6967651
• Country of Publication: United States
• Language: English

Related Subjects

640102* -- Astrophysics & Cosmology-- Stars & Quasi-Stellar
Radio & X-Ray Sources
640106 -- Astrophysics & Cosmology-- Cosmology
71 CLASSICAL AND QUANTUM MECHANICS
GENERAL PHYSICS
FIELD THEORIES
GENERAL RELATIVITY THEORY
GRAVITATIONAL RADIATION
NEUTRON STARS
OSCILLATIONS
PULSATIONS
RADIATIONS
SOLAR ACTIVITY
STARS