Large-amplitude isothermal fluctuations and high-density dark-matter clumps

Details Large-amplitude isothermal fluctuations and high-density dark-matter clumps Large-amplitude isothermal fluctuations and high-density dark-matter clumps

1994-03-07

arxiv.org/abs/astro-ph/9403011v1

Phys.Rev. D50 (1994) 769-773

Astronomy and Astrophysics

Astrophysics

15 pages plus 3 figures (included at the end as a uuencoded postscript file), LaTeX, FNAL--PUB--94/055--A

Scientific paper

10.1103/PhysRevD.50.769

Large-amplitude isothermal fluctuations in the dark matter energy density, parameterized by $\Phi\equiv\delta\rhodm/\rhodm$, are studied within the framework of a spherical collapse model. For $\Phi \ga 1$, a fluctuation collapses in the radiation-dominated epoch and produces a dense dark-matter object. The final density of the virialized object is found to be $\rho_F \approx 140\, \Phi^3 (\Phi+1) \rhoeq$, where $\rhoeq$ is the matter density at equal matter and radiation energy density. This expression is valid for the entire range of possible values of $\Phi$, both for $\Phi \gg 1$ and $\Phi \ll 1$. Some astrophysical consequences of high-density dark-matter clumps are discussed.

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