A Quantitative Study of Interacting Dark Matter in Halos
Open Access
- 10 November 2000
- journal article
- research article
- Published by American Astronomical Society in The Astrophysical Journal
- Vol. 543 (2) , 514-520
- https://doi.org/10.1086/317149
Abstract
We study the evolution of Hernquist profile "galaxies" in the presence of self-interacting dark matter (SIDM), where the properties of the dark matter can be parameterized by one number, DM = σDMMT/a2, for a halo of mass MT and break radius a. While the halos form constant-density cores of size ~a/2 on the core-radius relaxation timescale (trc 1.7tdyn/DM), core collapse begins shortly thereafter, and a steeper 1/r2 central density cusp starts forming faster than predicted by two-body relaxation. The formation of the steeper central cusp is accelerated if the cooling baryons adiabatically compress the dark matter. The natural consequence of SIDM is to exacerbate rather than to mitigate astrophysical problems created by dark matter density cusps.Keywords
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