Dark Lepton Superfluid in Proto-Neutron Stars. (arXiv:2107.06279v1 [hep-ph])
<a href="http://arxiv.org/find/hep-ph/1/au:+Reddy_S/0/1/0/all/0/1">Sanjay Reddy</a>, <a href="http://arxiv.org/find/hep-ph/1/au:+Zhou_D/0/1/0/all/0/1">Dake Zhou</a>
We find that sub-GeV neutrino portal bosons that carry lepton number can
condense inside a proto-neutron star (newly born neutron star). These bosons
are produced copiously and form a Bose-Einstein condensate for a range of as
yet unconstrained coupling strengths to neutrinos. The condensate is a lepton
number superfluid with transport properties that differ dramatically from those
encountered in ordinary dense baryonic matter. We discuss how this phase could
alter the evolution of proto-neutron stars and comment on the implications for
neutrino signals and nucleosynthesis.
We find that sub-GeV neutrino portal bosons that carry lepton number can
condense inside a proto-neutron star (newly born neutron star). These bosons
are produced copiously and form a Bose-Einstein condensate for a range of as
yet unconstrained coupling strengths to neutrinos. The condensate is a lepton
number superfluid with transport properties that differ dramatically from those
encountered in ordinary dense baryonic matter. We discuss how this phase could
alter the evolution of proto-neutron stars and comment on the implications for
neutrino signals and nucleosynthesis.
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