Fermionic Light Dark Matter Particles and the New Physics of Neutron Stars

Abstract

Dark Matter constitutes most of the matter in the presently accepted cosmological model for our Universe. The extreme conditions of ordinary baryonic matter, namely high density and compactness, in Neutron Stars make these objects suitable to gravitationally accrete such a massive component provided interaction strength between both, luminous and dark sectors, at current experimental level of sensitivity. We consider several different DM phenomenological models from the myriad of those presently allowed. In this contribution we review astrophysical aspects of interest in the interplay of ordinary matter and a fermionic light Dark Matter component. We focus in the interior nuclear medium in the core and external layers, i.e. the crust, discussing the impact of a novel dark sector in relevant stellar quantities for (heat) energy transport such as thermal conductivity or emissivities.

Dark halos around neutron stars and gravitational waves

“…If variability in the tidal deformability is detected in rare events it would imply that some fraction of neutron stars are able to capture large amounts of dark matter. Further, since neutron stars are not estimated to accrete nearly enough dark matter on the average to produce an observable gravitational wave signature if dark matter is distributed uniformly [47][48][49][50][51], discovering variability would have important implications for small scale structure in dark matter and hint at the existence of compact dark objects.…”

Radio telescope search for the resonant conversion of cold dark matter axions from the magnetized astrophysical sources

“…For instance, in the region where the neutron star distribution peaks in our galaxy (∼ a few kpc from the galactic center), the density can well be enhanced by more than an order of magnitude (e.g. ρ a ∼ O(10 ∼ 100) × 0.3GeV /cm 3 ) and could be even bigger ρ a ∼ O(10 4 ) × 0.3GeV /cm 3 around the neutron star found near the galactic center due to a dark matter spike [64][65][66][67][68][69][70].…”

Sneutrino Dark Matter in the BLSSM

“…All points obey the relic density upper limit, for which rescaling, where necessary, has been applied. 6 years of observation over 15 dSphs [76]. It should be noted that the assumed J-factor suffers from astrophysical uncertainties [77], but we do not consider any impact of these uncertainties within this study.…”

“…In fact, at present, the possibility of either scalar [1][2][3][4] or fermionic [5][6][7][8][9][10][11] DM is still allowed by observations. Among the possible candidates, Weakly Interactive Massive Particles (WIMP) are of special importance [12], since they can potentially be observable in direct detection [13][14][15][16][17], indirect detection [18,19] and collider experiments [20][21][22], in addition to the measurements of the WMAP [23] and Planck [24] satellites.…”