Effects of rotochemical heating on the thermal evolution of superfluid neutron stars HuaZhong Normal University Chun-Mei Pi & Xiao-Ping Zheng.

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Presentation transcript:

Effects of rotochemical heating on the thermal evolution of superfluid neutron stars HuaZhong Normal University Chun-Mei Pi & Xiao-Ping Zheng

Outline Equation of state and model of superfluidity Rotochemical heating The thermal evolution of NSs Conclusions

Equation of state Core: APR EOS Crust: BPS EOS

Model of nucleon superfluidity Gusakov et al.(2005),MNRAS,363,555

Rotochemical heating NS spin-down (decreasing centrifugal force) Chemical (“beta”) equilibrium sets relative number densities of particles (n, p, e, ...) at different pressures Compressing a fluid element perturbs equilibrium Non-equilibrium reactions tend to restore equilibrium “Chemical” energy released as neutrinos & “heat” Reisenegger 1995, ApJ, 442, 749

The neutrino emissivities & net reaction rates: Chemical imbalance: The neutrino emissivities & net reaction rates: The energy dissipation rate: Detailed model: Fernández & Reisenegger 2005, ApJ, 625, 291

The thermal evolution of NSs The energy and flux equations The thermal evolution equation with the approximation of isothermal interior

Three distinct cooling types : slow, moderate and fast cooling The transition from slow cooling to moderate one is sharp Neglecting the heating effects Gusakov et al.(2005),MNRAS,363,555

Taking the rotochemical heating into account The vacancy region will no longer exist Three distinct cooling types become ambiguous

Conclusions The rotochemical heating delays the cooling of superfluid neutron stars considerably . The picture of thermal evolution becomes completely different when including the rotochemical heating. The results are consistent with observations.

Thank you