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

Mar 1987

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987stin...8725108i&link_type=abstract

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Dark Matter, Density (Mass/Volume), Estimates, Galactic Nuclei, Angular Momentum, Cos-B Satellite, Radial Velocity

Scientific paper

The COS-B satellite observations of the cosmic gamma-ray flux are sensitive to gamma-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, higgsinos, sneutrinos 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 called the isothermal and adiabatic models. In the first, the dark matter is assumed to be isothermally distributed. In the second, 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 five too small. It is shown that, in the latter case, the density of dark matter particles near the center of the Galaxy is proportional to (-phic(r))3/2 where phic(r) is the gravitational potential due to the central component.

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