Constraints on scalar asymmetric dark matter from black hole formation in neutron stars

Abstract

We consider possibly observable effects of asymmetric dark matter (ADM) in neutron stars. Since dark matter does not self-annihilate in the ADM scenario, dark matter accumulates in neutron stars, eventually reaching the Chandrasekhar limit and forming a black hole. We focus on the case of scalar ADM, where the constraints from Bose-Einstein condensation and subsequent black hole formation are most severe due to the absence of Fermi degeneracy pressure. We also note that in some portions of this constrained parameter space, nontrivial effects from Hawking radiation can modify our limits. We find that for scalar ADM with mass between 5 MeV and 13 GeV, the constraint from nearby neutron stars on the scattering cross section with neutrons ranges from n & 10 À45 cm 2 to 10 À47 cm 2 .

Realistic neutron star constraints on bosonic asymmetric dark matter

“…Thus, the estimate of Eq. (10) suggests that 4 takes values many orders of magnitude greater than is necessary to prevent gravitational collapse of light bosonic ADM in neutron stars. 5 The formation of a DM Bose-Einstein condensate is necessary for gravitational collapse (see Refs.…”

“…[10]). In this mass range, a black hole would be expected to form in the core of neutron stars located in the Milky Way within their observed lifetime.…”

“…Observations of stellar objects have been employed to constrain the properties of ADM [6][7][8][9][10][11][12]. If DM interacts with nuclear matter, then it can scatter on the nucleons in compact objects, lose energy, and become captured in their interiors [13,14].…”

Dark matter induced nucleon decay: model and signatures

“…Further, the nucleon number density of the stellar object is usually much higher than matter on the Earth, one expects the IND process happens much more frequently. Here we want to emphasize that in [69][70][71][72], one constrains the scalar asymmetric DM models by requiring that the accumulation of DM in neutron star does not cause a black hole in the core. In our model, since DM can annihilate with nucleons, and the anit-DM in the final state of IND process can further annihilate with DM, the accumulation of DM in the neutron star is not efficient enough to form a black hole.…”

Spontaneous baryogenesis from extremely light asymmetric dark matter

“…Furthermore current direct detection experiments sensitive to low mass WIMPS such as DAMIC [59], CDMSLite [60], LUX [61], Xenon10 [62] and SuperCDMS [63] do not place constraints on dark matter masses below a GeV. Note that neutron star bounds on scalar asymmetric dark matter could already exclude the range of interest for direct detection [64]. Since the dark matter could be captured and reach densities large enough to create a black hole during 6 Note that for an abelian symmetry, using charges that are orders of magnitude away from each other the appearance of new physics can be delayed up to Λ N P .…”