Contribution of the massive photon decay channel to neutrino cooling of neutron stars

Abstract

We consider massive photon decay reactions via intermediate states of electron-electron-holes and proton-proton-holes into neutrino-antineutrino pairs in the course of neutron star cooling. These reactions may become operative in hot neutron stars in the region of proton pairing where the photon due to the Higgs-Meissner effect acquires an effective mass $m_{\gamma }$ that is small compared to the corresponding plasma frequency. The contribution of these reactions to neutrino emissivity is calculated; it varies with the temperature and the photon mass as $T^{3/2}{m}_{\gamma }^{7/2}{e}^{-m_{\gamma }/T}$ for $T<m_{\gamma }$. Estimates show that these processes appear as extra efficient cooling channels of neutron stars at temperatures $T\simeq (10^9-10^{10})$ K.

accepted to publication in Zh. Eksp. Teor. Fiz. (JETP)

Cited by in corpus (6)

• Diquark Condensates and Compact Star Cooling
• Cooling of Neutron Stars. Hadronic Model
• Neutrino emission due to Cooper-pair recombination in neutron stars revisited
• Nuclear medium cooling scenario in the light of new Cas A cooling data and the 2 M_sun pulsar mass measurements
• Medium Effects in Cooling of Neutron Stars and $3P_2$ Neutron Gap
• Medium effects in the pion pole mechanism (photon photon --> pion-zero --> neutrino-R antineutrino-L (neutrino-L antineutrino-R)) of neutron star cooling