Estimates of the density of dark matter near the center of the Galaxy

Details Estimates of the density of dark matter near the center of the Galaxy Estimates of the density of dark matter near the center of the Galaxy

Jun 1987

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987phrvd..35.3695i&link_type=abstract

Physical Review D (Particles and Fields), Volume 35, Issue 12, 15 June 1987, pp.3695-3704

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37

Origin And Formation Of The Universe

Scientific paper

It was recently pointed out by Silk and Bloemen that the COS-B satellite observations of the cosmic γ-ray flux are sensitive to γ rays from dark-matter annihilation at the center of the Galaxy if the dark matter is composed of stable weakly interacting particles such as photinos, Higgs fermions, scalar neutrinos, or heavy neutrinos and if the dark-matter content of the central component of the Galaxy is more than about 2%. Motivated by this remark, we have studied how much dark matter is expected to be near the center of the Galaxy under two different assumptions which we call the isothermal and adiabatic models. In the first model, the dark matter is assumed to be isothermally distributed. In the second model, it is assumed that while the central component forms the adiabatic invariant for the radial motion of each dark-matter particle, as well as its angular momentum, is conserved. In the isothermal model, the typical dark-matter density enhancement near the center of the Galaxy is large enough to make the COS-B data sensitive to the hypothesis that the dark matter is composed of stable weakly interacting particles, whereas in the adiabatic model it is about a factor of 5 too small. We show that in the adiabatic model the density of dark-matter particles near the center of the Galaxy is proportional to [-φc(r)]3/2 where φc(r) is the gravitational potential due to the central component.

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