Quark matter contribution to the heat capacity of magnetized neutron stars
arXiv:2101.04032 · doi:10.1103/PhysRevD.103.123013
Abstract
In this paper, we find the heat capacity of the magnetic dual chiral density wave (MDCDW) phase of dense quark matter and use it to explore the feasibility of this phase for a neutron star interior. MDCDW is a spatially inhomogeneous phase of quark matter known to be favored at intermediate densities over the chirally symmetric phase and the color-flavor-locked superconducting phase. By comparing our result to the lower limit of the core heat capacity established from observations of transiently accreting neutron stars, we show that the heat capacity of MDCDW quark matter is well above that lower limit and hence cannot be ruled out. This result adds to a wealth of complementary investigations, all of which has served to strengthen the viability of a neutron star interior made of MDCDW quark matter. For completeness, we review the contributions to the heat capacity of the main neutron star ingredients at low, high and intermediate densities, with and without the presence of a magnetic field.
To appear in PRD
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Cited by in corpus (8)
- Phase transitions and resilience of the MDCDW phase at finite temperature and density
- Speed of Sound for Hadronic and Quark Phases in a Magnetic Field
- Axion-Polaritons in the Magnetic Dual Chiral Density Wave Phase of Dense QCD
- Effect of anomalous magnetic moment on the chiral transition at zero temperature in a strong magnetic field
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- Axion-Polaritons in quark stars: a possible solution to the missing pulsar problem
- Casimir effect in magnetic dual chiral density waves
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