A dark matter scaling relation from mirror dark matter

Abstract

Mirror dark matter, and other similar dissipative dark matter candidates, need an energy source to stabilize dark matter halos in spiral galaxies. It has been suggested previously that ordinary supernovae can potentially supply the required energy. By matching the energy supplied to the halo from supernovae to that lost due to radiative cooling, we here derive a rough scaling relation, $R_{SN}\propto {\rho }_0{r}_0^2$ ($R_{SN}$ is the supernova rate and ${\rho }_0,r_0$ the dark matter central density and core radius). Such a relation is consistent with dark matter properties inferred from studies of spiral galaxies with halo masses larger than $3\times 10^{11}{M}_{\odot }$. We speculate that other observed galaxy regularities might be explained within the framework of such dissipative dark matter.

About 10 pages, some adjustments

References in corpus (3)

• Results from a Search for Light-Mass Dark Matter with a P-type Point Contact Germanium Detector
• Mirror dark matter and the new DAMA/LIBRA results: A simple explanation for a beautiful experiment
• Galactic structure explained with dissipative mirror dark matter

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• Mirror dark matter: Cosmology, galaxy structure and direct detection
• Galactic structure explained with dissipative mirror dark matter
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• Dissipative dark matter explains rotation curves