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Hybrid stars with the Dyson-Schwinger quark model
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Hybrid stars with the Dyson-Schwinger quark model
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We study the hadron-quark phase transition in the interior of neutron stars. For the hadronic sector, we use a microscopic equation of state involving nucleons and hyperons derived within the Brueckner-Hartree-Fock many-body theory with realistic two-body and three-body forces. For the description of quark matter, we employ the Dyson-Schwinger approach and compare with the MIT bag model. We calculate the structure of neutron star interiors comprising both phases and find that with the Dyson-Schwinger model, the hadron-quark phase transition takes place only when hyperons are excluded, and that a two-solar-mass hybrid star is possible only if the nucleonic equation of state is stiff enough.
Forward citations
Cited by 2 Pith papers
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Cooling of Hybrid Stars with a 2SC+$<dd>$ Phase
Hybrid stars containing the 2SC+<dd> phase cool more slowly than those with the 2SC phase because inherited 3P2 superfluidity suppresses quark beta decay, producing cooling curves close to the CFL case.
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Cooling of Hybrid Stars with a 2SC+$<dd>$ Phase
Hybrid stars with a 2SC+⟨dd⟩ quark core cool hotter than with 2SC and near CFL; with a 3P2 gap near 5×10^8 K their cooling curves pass through the observed temperatures of 3C58, Vela Jr., and Vela-like pulsars.
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