Galactic Constraints on Fermionic Dark Matter


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Abstract

In order to explain Galactic structures, a self-gravitating system composed of massive fermions in spherical symmetry is considered. The finite mass distribution of such a component is obtained after solving the Einstein equation for a thermal and semi-degenerate fermionic gas, described by a perfect fluid in hydrostatic equilibrium and exposed to cutoff effects (e.g. evaporation). Within this more general approach a family of density profiles arises, which explains dark matter halo constraints of the Galaxy and provides at the same time an alternative to the central black hole scenario in Sgr A*. This analysis narrows the allowed particle mass to mc2 = 48−345 keV.

About the authors

A. Krut

ICRANet; ICRA and University of Rome “Sapienza,”; University of Nice-Sophia Antipolis

Author for correspondence.
Email: andreas.krut@gmx.de
Italy, Pescara; Rome; Nice

C. R. Arguëlles

ICRANet; Instituto de Astrofisica de La Plata (CCT La Plata, CONICET, UNLP)

Email: andreas.krut@gmx.de
Italy, Pescara; La Plata

J. Rueda

ICRANet; ICRA and University of Rome “Sapienza,”; ICRANet-Rio

Email: andreas.krut@gmx.de
Italy, Pescara; Rome; Rio de Janeiro

R. Ruffini

ICRANet; ICRA and University of Rome “Sapienza,”; ICRANet-Rio

Email: andreas.krut@gmx.de
Italy, Pescara; Rome; Rio de Janeiro

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