Abstract
Neutron stars change their structure with accumulation of dark matter. We study how their mass is influenced from the environment. Close to the sun, the dark matter accretion from the neutron star does not have any effect on it. Moving towards the galactic center, the density increase in dark matter results in increased accretion. At distances of some fraction of a parsec, the neutron star acquire enough dark matter to have its structure changed. We show that the neutron star mass decreases going towards the galactic centre, and that dark matter accumulation beyond a critical value collapses the neutron star into a black hole. Calculations cover cases varying the dark matter particle mass, self-interaction strength, and ratio between the pressure of dark matter and ordinary matter. This allow us to constrain the interaction cross section, σdm, between nucleons and dark matter particles, as well as the dark matter self-interaction cross section.
Highlights
Explaining structure formation without the need to modify gravity in current cosmological models entails the introduction of dark matter (DM)
The larger the mass acquired by the Neutron stars (NSs), the smaller its maximal total mass, it is expected that going towards the galactic center (GC), or if we are in the center of dark matter clumps, the NSs mass must be smaller than that in an environment without DM
Since we found that more DM is captured in the Compact Objects (COs) if the DM particle mass is smaller, we constrained from 2 M observations the amount of DM capture
Summary
Explaining structure formation without the need to modify gravity in current cosmological models entails the introduction of dark matter (DM). For a larger accumulated DM amount than a critical value [35], the resulting NS could collapse into a mini black-hole This allows us to constrain further the cross section and mass of the DM particles [29]. The larger the mass acquired by the NS, the smaller its maximal total mass, it is expected that going towards the GC, or if we are in the center of dark matter clumps, the NSs mass must be smaller than that in an environment without DM This property is used to put constraints on the interaction cross-sections for nucleon-dark matter and DM–DM self interaction.
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