Franz E. Schunck
Fjodor V. Kusmartsev
Eckehard W. Mielke
Publisher: Cambridge University Press
Print Publication Year: 1992
Online Publication Date:December 2009
Online ISBN:9780511524639
Hardback ISBN:9780521439763
Paperback ISBN:9780521017350
Chapter DOI: http://dx.doi.org/10.1017/CBO9780511524639.015
Subjects: Cosmology, Relativity and Gravitation, Astrophysics
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Abstract. We investigate the stability of charged boson stars in the framework of general relativity. The constituents of these stars are scalar bosons which interact not only via their charge and mass but also via a short–range Higgs potential U. Our stability analysis is based on catastrophe theory which is capable of providing more information than perturbation theory. In fact, it predicts novel oscillation and collapse regimes for a certain range of the particle number.
INTRODUCTION
In the early universe, spin-zero particles, such as the scalar Higgs particles, may have played an important rôle [1]. At that early time it is conceivable that clouds of particles created stars which are kept together by their own gravitational field, the so–called boson stars [2]. These stars could make up a considerable fraction of the hypothetical dark matter.
The boson star consists of many particles and may have a very large mass comparable or larger than that of a neutron star. The latter depends upon the form of a self–interaction between the bosons [3]. Generally speaking, the boson star is in many ways analogous to the neutron star [4,5]. Both stars consist of one matter component. Recently, Higgs particles interacting with gauge field have been studied [6]. If we attribute charge to the bosons, they will interact also via electromagnetic forces. Because of the repulsive nature of this interaction there exists a critical total charge of these scalar particles beyond which the star becomes unstable [6].
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PART A - THEORETICAL APPROACHES: Read PDF
pp. 1-2
Numerical relativity on a transputer array: Read PDF
pp. 3-19
Some aspects of the characteristic initial value problem in numerical relativity: Read PDF
pp. 20-33
The characteristic initial value problem in general relativity: Read PDF
pp. 34-40
Algebraic approach to the characteristic initial value problem in general relativity: Read PDF
pp. 41-49
On hyperboloidal hypersurfaces: Read PDF
pp. 50-58
The initial value problem on null cones: Read PDF
pp. 59-68
Introduction to dual-null dynamics: Read PDF
pp. 69-78
On colliding plane wave space-times: Read PDF
pp. 79-82
Boundary conditions for the momentum constraint: Read PDF
pp. 83-93
On the choice of matter model in general relativity: Read PDF
pp. 94-102
A mathematical approach to numerical relativity: Read PDF
pp. 103-113
Making sense of the effects of rotation in general relativity: Read PDF
pp. 114-129
Stability of charged boson stars and catastrophe theory: Read PDF
pp. 130-140
PART B - PRACTICAL APPROACHES: Read PDF
pp. 141-142
Numerical asymptotics: Read PDF
pp. 143-162
Instabilities in rapidly rotating polytropes: Read PDF
pp. 163-181
Gravitational radiation from coalescing binary neutron stars: Read PDF
pp. 182-201
“Critical” behaviour in massless scalar field collapse: Read PDF
pp. 202-222
Godunov-type methods applied to general relativistic stellar collapse: Read PDF
pp. 223-229
Astrophysical sources of gravitational waves and neutrinos: Read PDF
pp. 230-246
Gravitational radiation from 3D gravitational stellar core collapse: Read PDF
pp. 247-257
A vacuum fully relativistic 3D numerical code: Read PDF
pp. 258-264
Solution of elliptic equations in numerical relativity using multiquadrics: Read PDF
pp. 265-280
Self-gravitating thin discs around rotating black holes: Read PDF
pp. 281-291
An ADI scheme for a black hole problem: Read PDF
pp. 292-296
Time-symmetric ADI and causal reconnection: Read PDF
pp. 297-307
The numerical study of topological defects: Read PDF
pp. 308-334
Computations of bubble growth during the cosmological quark-hadron transition: Read PDF
pp. 335-344
Initial data of axisymmetric gravitational waves with a cosmological constant: Read PDF
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