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.
Tests of the nuclear equation of state and superfluid and superconducting gaps using the Cassiopeia A neutron star
2 Pith papers cite this work. Polarity classification is still indexing.
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abstract
The observed rapid cooling of the Cassiopeia A neutron star can be interpreted as being caused by neutron and proton transitions from normal to superfluid and superconducting states in the stellar core. Here we present two new Chandra ACIS-S Graded observations of this neutron star and measurements of the neutron star mass M and radius R found from consistent fitting of both the X-ray spectra and cooling behavior. This comparison is only possible for individual nuclear equations of state. We test phenomenological superfluid and superconducting gap models which mimic many of the known theoretical models against the cooling behavior. Our best-fit solution to the Cassiopeia A data is one in which the (M,R) = (1.44 Msun,12.6 km) neutron star is built with the BSk21 equation of state, strong proton superconductor and moderate neutron triplet superfluid gap models, and a pure iron envelope or a thin carbon layer on top of an iron envelope, although there are still large observational and theoretical uncertainties.
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2026 2verdicts
UNVERDICTED 2representative citing papers
Bayesian analysis of generic hybrid EOS with first-order deconfinement shows mass-gap hybrids require early transition and stiff quark matter, but data favor twins at 1.4 M_sun that exclude them.
citing papers explorer
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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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Hybrid stars among mass gap objects are excluded by twin stars at $1.4\,M_\odot$
Bayesian analysis of generic hybrid EOS with first-order deconfinement shows mass-gap hybrids require early transition and stiff quark matter, but data favor twins at 1.4 M_sun that exclude them.