Self-similar spherical collapse with non-radial motions

Details Self-similar spherical collapse with non-radial motions Self-similar spherical collapse with non-radial motions

2000-08-15

arxiv.org/abs/astro-ph/0008217v1

Mon.Not.Roy.Astron.Soc. 325 (2001) 1397

Astronomy and Astrophysics

Astrophysics

6 pages, 1 figure, two column MNRAS style

Scientific paper

10.1046/j.1365-8711.2001.04527.x

We derive the asymptotic mass profile near the collapse center of an initial spherical density perturbation, $\delta \propto M^{-\epsilon}$, of collision-less particles with non-radial motions. We show that angular momenta introduced at the initial time do not affect the mass profile. Alternatively, we consider a scheme in which a particle moves on a radial orbit until it reaches its turnaround radius, r_*. At turnaround the particle acquires an angular momentum $L={\cal L} \sqrt{GM_* r_*}$ per unit mass, where M_* is the mass interior to r_*. In this scheme, the mass profile is $M\propto r^{3/(1+3\epsilon)}$ for all $\epsilon >0$, in the region $r/r_t\ll {\cal L}$, where r_t is the current turnaround radius. If ${\cal L} \ll 1$ then the profile in the region ${\cal L} \ll r/r_t \ll$ is $M\propto r$ for $\epsilon <2/3$. The derivation relies on a general property of non-radial orbits which is that ratio of the pericenter to apocenter is constant in a force field k(t) r^{n} with k(t) varying adiabatically.

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