Nucleon Structure and Strong Interactions in Dark Matter Capture in Neutron Stars. (arXiv:2012.08918v2 [hep-ph] UPDATED)
<a href="http://arxiv.org/find/hep-ph/1/au:+Bell_N/0/1/0/all/0/1">Nicole F. Bell</a>, <a href="http://arxiv.org/find/hep-ph/1/au:+Busoni_G/0/1/0/all/0/1">Giorgio Busoni</a>, <a href="http://arxiv.org/find/hep-ph/1/au:+Motta_T/0/1/0/all/0/1">Theo F. Motta</a>, <a href="http://arxiv.org/find/hep-ph/1/au:+Robles_S/0/1/0/all/0/1">Sandra Robles</a>, <a href="http://arxiv.org/find/hep-ph/1/au:+Thomas_A/0/1/0/all/0/1">Anthony W. Thomas</a>, <a href="http://arxiv.org/find/hep-ph/1/au:+Virgato_M/0/1/0/all/0/1">Michael Virgato</a>

We outline two important effects that are missing from most evaluations of
the dark matter capture rate in neutron stars. As dark matter scattering with
nucleons in the star involves large momentum transfer, nucleon structure must
be taken into account via a momentum dependence of the hadronic form factors.
In addition, due to the high density of neutron star matter, we should account
for nucleon interactions rather than modeling the nucleons as an ideal Fermi
gas. Properly incorporating these effects is found to suppress the dark matter
capture rate by up to three orders of magnitude for the heaviest stars.

We outline two important effects that are missing from most evaluations of
the dark matter capture rate in neutron stars. As dark matter scattering with
nucleons in the star involves large momentum transfer, nucleon structure must
be taken into account via a momentum dependence of the hadronic form factors.
In addition, due to the high density of neutron star matter, we should account
for nucleon interactions rather than modeling the nucleons as an ideal Fermi
gas. Properly incorporating these effects is found to suppress the dark matter
capture rate by up to three orders of magnitude for the heaviest stars.

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