Within this nucleon-meson model, a chiral density wave in neutron star cores is only stable for equations of state too soft to support observed two-solar-mass pulsars, predicting isotropic cores.
Quark beta decay in the inhomogeneous chiral phase and cooling of compact stars
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abstract
A novel cooling mechanism is proposed for neutron stars, based on the recent development in the studies of the QCD phase diagram. Possible appearance of the inhomogeneous chiral phase makes the quark beta decay without gluonic interaction. An estimate of the neutrino emissivity shows the order of $10^{24-26}(T/10^9)^6$(erg cm$^{-3}$ s$^{-1}$) near the phase boundaries, whose efficiency is comparable with the usual quark cooling or pion cooling, but it works only in the limited density region. These features may give another cooling scenario of neutron stars.
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How neutron star properties disfavor a nuclear chiral density wave
Within this nucleon-meson model, a chiral density wave in neutron star cores is only stable for equations of state too soft to support observed two-solar-mass pulsars, predicting isotropic cores.