Self-similar growth of primordial black holes. I. Stiff equation of state
We discuss the possible self-similar growth of primordial black holes in a ''stiff'' early Universe. We conclude that such growth is possible only if the black hole accretes the matter as a null-fluid inside a certain surface, called here the phase-change surface. This has required us to match an ingoing self-similar Vaidya solution to the self-similar p=epsilon matter solution. We also discuss carefully the rarefaction waves that play an essential role in the accretion flow.Numerically we agree with an earlier result by Lin et al., that the maximum mass reached by primordial black holes in the stiff era is 1 M/sub sun/. However, our description of the process is quite different from theirs. Moreover, we feel that whether there is rapid growth of black holes in softer epochs of the Universe is as yet undecided, pending a proper discussion of the weak discontinuities (critical points) in the self-similar flow.
- Research Organization:
- Astronomy Group, Queen's University at Kingston, Ontario
- OSTI ID:
- 5036223
- Journal Information:
- Astrophys. J.; (United States), Vol. 219:3
- Country of Publication:
- United States
- Language:
- English
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Related Subjects
GENERAL PHYSICS
BLACK HOLES
EQUATIONS OF STATE
COSMOLOGICAL MODELS
COSMOLOGY
EINSTEIN FIELD EQUATIONS
FLUID FLOW
NUCLEONS
SHOCK WAVES
STAR ACCRETION
UNIVERSE
BARYONS
ELEMENTARY PARTICLES
EQUATIONS
FERMIONS
FIELD EQUATIONS
HADRONS
MATHEMATICAL MODELS
STAR EVOLUTION
640102* - Astrophysics & Cosmology- Stars & Quasi-Stellar
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