The prospects for indirect detection of dark matter at the Galactic center with gamma-ray experiments like the space telescope GLAST, and Air Cherenkov Telescopes like HESS, CANGAROO, MAGIC and VERITAS, depend sensitively on the mass profile within the inner parsec. We calculate the distribution of dark matter on sub-parsec scales by integrating the time-dependent Fokker-Planck equation, including the effects of self-annihilations, scattering of dark matter particles by stars, and capture in the supermassive black hole. We consider a variety of initial dark matter distributions, including models with very high densities (“spikes”) near the black hole, and models with “adiabatic compression” of the baryons. The annihilation signal after 1010 yr is found to be substantially reduced from its initial value, but in dark matter models with an initial spike, order-of-magnitude enhancements can persist compared with the rate in spike-free models.

Publication Date



Also archived In: arXiv: astro-ph/0501555 v2 17 Oct 2005 This work was supported by grants AST-0071099, AST-0206031, AST-0420920 and AST-0437519 from the NSF, grant NNG04GJ48G and NAG 5-10842 from NASA, and grant HST-AR-09519.01-A from STScI. Note: imported from RIT’s Digital Media Library running on DSpace to RIT Scholar Works in February 2014.

Document Type


Department, Program, or Center

School of Physics and Astronomy (COS)


RIT – Main Campus