Ming-Feng Zhu

The Nucleon Direct Urca Processes in a Cooling Neutron Star

In the relativistic mean field approximation, the relativistic energy losses of the nucleon direct Urca processes are studied in the degenerate baryon matter of neutron stars. We investigate the effects of hyperon degrees of freedom and the isovector scalar interaction which is considered by exchanging delta meson on the nucleon direct Urca processes in neutron star matter. The results indicate that the existence of hyperons decreases the abundance of protons and leptons and can sharply suppress the neutrino emissivity of the nucleon direct Urca processes, while it has only a little influence on the neutrino luminosity for a fixed neutron star whether delta mesons appear in a neutron star or not. However, the presence of delta mesons can result in obvious growth in the neutrino emissivity and luminosity which will speed up the cooling rate for the nonsuperfluid neutron star.

Singlet pairing gaps of neutrons and protons in hyperonic neutron stars

The

The influence of antikaon condensations on neutrino emissivity from neutron stars

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Self-consistently thermodynamic treatment for strange quark matter in the effective mass bag model

nucleonic superfluids are investigated within the relativistic mean-field model and Bardeen-Cooper-Schrieffer theory in hyperonic neutron stars. The

Direct Urca processes involving hyperons in neutron star matter

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The third family of compact stars with the color-flavor locked quark core

pairing gaps of neutrons and protons are calculated based on the Reid soft-core interaction as the nucleon-nucleon interaction. We have studied particularly the influence of hyperons degrees of freedom on the

Thermal neutron stars including the hyperon-hyperon interactions

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1S0Nucleon Superfluidity in Neutron Star Matter

nucleonic pairing gap in neutron star matter. It is found that the appearance of hyperons has little impact on baryonic density range and size for the

NUCLEAR PHYSICS: bar K Condensation in Neutron Star Matter with Delta Quartet

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K Condensation in Neutron Star Matter with ? Quartet

neutronic pairing gap, the