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Abstract
The short distance behavior of dark matter (DM) at galaxy scales exhibits several features not explained by the typical cold dark matter (CDM) with velocity-independent cross-section. We discuss a particle physics model with a hidden sector interacting feebly with the visible sector where a dark fermion self-interacts via a dark force with a light dark photon as the mediator. We study coupled Boltzmann equations involving two temperatures, one for each sector. We fit the velocity-dependent DM cross-section to the data from scales of dwarf galaxies to clusters consistent with relic density constraint.
Highlights
While the Lambda cold dark matter (ΛCDM) model works very well at large scales, several issues have arisen recently concerning weakly interacting massive particles (WIMPs) as CDM with regards to physics at galaxy scales
New analytic results of this work are the three coupled equations defined by Eqs. (24)–(28) which allow one to solve the Boltzmann equations for the relic density of dark matter where the evolution depends on two temperatures, one for the hidden and the other for the visible sector
The analysis shows that thermalization of the hidden sector occurs for all the model points and the more feeble the interaction is the longer it takes for thermalization to occur
Summary
While the Lambda cold dark matter (ΛCDM) model works very well at large scales, several issues have arisen recently concerning weakly interacting massive particles (WIMPs) as CDM with regards to physics at galaxy scales. Some of these are described as the cusp core, the missing satellites, and the too-big-to-fail (TBTF) anomalies. Because the mass of the third neutral boson would turn out to be in MeV region we will refer to it as a dark photon or γ0 which, is unstable and decays
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