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Relativistic Stellar Pulsations

Citation

Finn, Lee Samuel (1987) Relativistic Stellar Pulsations. Dissertation (Ph.D.), California Institute of Technology. http://resolver.caltech.edu/CaltechETD:etd-08262008-093129

Abstract

This thesis consists of studies on the topic of relativistic stellar pulsations.

i) 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 formalism is used to study g-modes that arise because of chemical inhomogeneities in neutron star crusts. g-mode frequencies associated with chemical inhomogeneities are found to be much higher than those associated with finite temperature.

ii) The relativistic Cowling approximation, introduced by McDermott, Van Horn, and Scholl (1983) and 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.

iii) Realistic neutron stars have a solid crust, and this will seriously affect their g-modes. The first steps toward developing a theory of non-radial relativistic pulsations in stars with a solid crust is reported on here: the calculation of the shear strain and stress during a pulsation, the introduction of the shear stress into the Einstein field equations as a source and to the equations of motion as a force, and the development of a Lagrangian and variational principle for studying non-radial relativistic pulsations in stars with a solid crust.

iv) 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." The transition-zone gravitational field is explored for four relativistic gravity theories: a spin-zero theory (Nordstøm's theory), a spin-one theory (analogous to electromagnetism), a spin-two theory (general relativity), and a mixed spin-zero/spin-one theory (Jordan-Brans-Dicke theory). From the transition-zone gravitational field, it is possible to determine experimentally the spin content of relativistic gravity.

Item Type:Thesis (Dissertation (Ph.D.))
Subject Keywords:Stellar pulsations; neutron stars; gravitational waves
Degree Grantor:California Institute of Technology
Division:Physics, Mathematics and Astronomy
Major Option:Physics
Thesis Availability:Public (worldwide access)
Research Advisor(s):
  • Thorne, Kip S.
Group:TAPIR
Thesis Committee:
  • Thorne, Kip S. (chair)
  • Phinney, E. Sterl
  • Libbrecht, Kenneth George
  • Zachariasen, Fredrik
Defense Date:11 May 1987
Non-Caltech Author Email:lsfinn (AT) psu.edu
Funders:
Funding AgencyGrant Number
CaltechUNSPECIFIED
Record Number:CaltechETD:etd-08262008-093129
Persistent URL:http://resolver.caltech.edu/CaltechETD:etd-08262008-093129
Related URLs:
URLURL TypeDescription
https://doi.org/10.1093/mnras/222.3.393DOIArticle adapted for Chapter 2.
https://doi.org/10.1093/mnras/227.2.265DOIArticle adapted for Chapter 3.
https://doi.org/10.1093/mnras/232.2.259DOIArticle adapted for Chapter 4.
https://doi.org/10.1088/0264-9381/2/3/014DOIArticle adapted for Chapter 6.
Default Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:3230
Collection:CaltechTHESIS
Deposited By: Imported from ETD-db
Deposited On:09 Sep 2008
Last Modified:27 Jun 2019 17:29

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