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.
Department, Program, or Center
School of Physics and Astronomy (COS)
G. Bertone and D. Merritt, Phys. Rev. D 72, 103502 (2005). https://doi.org/10.1103/PhysRevD.72.103502
RIT – Main Campus