Quark deconfinement in compact stars through sexaquark condensation. (arXiv:2202.05061v2 [nucl-th] UPDATED)
<a href="http://arxiv.org/find/nucl-th/1/au:+Blaschke_D/0/1/0/all/0/1">D. Blaschke</a>, <a href="http://arxiv.org/find/nucl-th/1/au:+Ivanytskyi_O/0/1/0/all/0/1">O. Ivanytskyi</a>, <a href="http://arxiv.org/find/nucl-th/1/au:+Shahrbaf_M/0/1/0/all/0/1">M. Shahrbaf</a>
In this contribution, we present for the first time a scenario according to
which early quark deconfinement in compact stars is triggered by the
Bose-Einstein condensation (BEC) of a light sexaquark (S) with a mass
$m_S<2054$ MeV, that has been suggested as a candidate particle to explain the
baryonic dark matter in the Universe. The onset of S BEC marks the maximum mass
of hadronic neutron stars and it occurs when the condition for the baryon
chemical potential $mu_b=m_S/2$ is fulfilled in the center of the star,
corresponding to $M_{rm onset}lesssim 0.7~M_odot$. In the gravitational
field of the star the density of the BEC of the S increases until a new state
of the matter is attained, where each of the S-states got dissociated into a
triplet of color-flavor-locked (CFL) diquark states. These diquarks are the
Cooper pairs in the color superconducting CFL phase of quark matter, so that
the developed scenario corresponds to a BEC-BCS transition in strongly
interacting matter. For the description of the CFL phase, we develop here for
the first time the three-flavor extension of the density-functional formulation
of a chirally symmetric Lagrangian model of quark matter where confining
properties are encoded in a divergence of the scalar self-energy at low
densities and temperatures.
In this contribution, we present for the first time a scenario according to
which early quark deconfinement in compact stars is triggered by the
Bose-Einstein condensation (BEC) of a light sexaquark (S) with a mass
$m_S<2054$ MeV, that has been suggested as a candidate particle to explain the
baryonic dark matter in the Universe. The onset of S BEC marks the maximum mass
of hadronic neutron stars and it occurs when the condition for the baryon
chemical potential $mu_b=m_S/2$ is fulfilled in the center of the star,
corresponding to $M_{rm onset}lesssim 0.7~M_odot$. In the gravitational
field of the star the density of the BEC of the S increases until a new state
of the matter is attained, where each of the S-states got dissociated into a
triplet of color-flavor-locked (CFL) diquark states. These diquarks are the
Cooper pairs in the color superconducting CFL phase of quark matter, so that
the developed scenario corresponds to a BEC-BCS transition in strongly
interacting matter. For the description of the CFL phase, we develop here for
the first time the three-flavor extension of the density-functional formulation
of a chirally symmetric Lagrangian model of quark matter where confining
properties are encoded in a divergence of the scalar self-energy at low
densities and temperatures.
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