Three types of cooling superfluid neutron stars : Theory and observations

@inproceedings{Kaminker2001ThreeTO,
  title={Three types of cooling superfluid neutron stars : Theory and observations},
  author={Alexander Kaminker and Dmitry G. Yakovlev and Oleg Y. Gnedin},
  year={2001}
}
Cooling of neutron stars (NSs) with the cores composed of neutrons, protons, and electrons is simulated assuming S0 pairing of neutrons in the NS crust, and also S0 pairing of protons and weak P2 pairing of neutrons in the NS core, and using realistic density profiles of the superfluid critical temperatures Tc(ρ). The theoretical cooling models of isolated middle-aged NSs can be divided into three main types. (I) Low-mass, slowly cooling NSs where the direct Urca process of neutrino emission is… CONTINUE READING

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Cooling of neutron stars ( NSs ) with the cores composed of neutrons , protons , and electrons is simulated assuming S0 pairing of neutrons in the NS crust , and also S0 pairing of protons and weak P2 pairing of neutrons in the NS core , and using realistic density profiles of the superfluid critical temperatures Tc(ρ ) .
Cooling of neutron stars ( NSs ) with the cores composed of neutrons , protons , and electrons is simulated assuming S0 pairing of neutrons in the NS crust , and also S0 pairing of protons and weak P2 pairing of neutrons in the NS core , and using realistic density profiles of the superfluid critical temperatures Tc(ρ ) .
Cooling of neutron stars ( NSs ) with the cores composed of neutrons , protons , and electrons is simulated assuming S0 pairing of neutrons in the NS crust , and also S0 pairing of protons and weak P2 pairing of neutrons in the NS core , and using realistic density profiles of the superfluid critical temperatures Tc(ρ ) .
Cooling of neutron stars ( NSs ) with the cores composed of neutrons , protons , and electrons is simulated assuming S0 pairing of neutrons in the NS crust , and also S0 pairing of protons and weak P2 pairing of neutrons in the NS core , and using realistic density profiles of the superfluid critical temperatures Tc(ρ ) .
Cooling of neutron stars ( NSs ) with the cores composed of neutrons , protons , and electrons is simulated assuming S0 pairing of neutrons in the NS crust , and also S0 pairing of protons and weak P2 pairing of neutrons in the NS core , and using realistic density profiles of the superfluid critical temperatures Tc(ρ ) .
Cooling of neutron stars ( NSs ) with the cores composed of neutrons , protons , and electrons is simulated assuming S0 pairing of neutrons in the NS crust , and also S0 pairing of protons and weak P2 pairing of neutrons in the NS core , and using realistic density profiles of the superfluid critical temperatures Tc(ρ ) .
Cooling of neutron stars ( NSs ) with the cores composed of neutrons , protons , and electrons is simulated assuming S0 pairing of neutrons in the NS crust , and also S0 pairing of protons and weak P2 pairing of neutrons in the NS core , and using realistic density profiles of the superfluid critical temperatures Tc(ρ ) .
Cooling of neutron stars ( NSs ) with the cores composed of neutrons , protons , and electrons is simulated assuming S0 pairing of neutrons in the NS crust , and also S0 pairing of protons and weak P2 pairing of neutrons in the NS core , and using realistic density profiles of the superfluid critical temperatures Tc(ρ ) .
Cooling of neutron stars ( NSs ) with the cores composed of neutrons , protons , and electrons is simulated assuming S0 pairing of neutrons in the NS crust , and also S0 pairing of protons and weak P2 pairing of neutrons in the NS core , and using realistic density profiles of the superfluid critical temperatures Tc(ρ ) .
Cooling of neutron stars ( NSs ) with the cores composed of neutrons , protons , and electrons is simulated assuming S0 pairing of neutrons in the NS crust , and also S0 pairing of protons and weak P2 pairing of neutrons in the NS core , and using realistic density profiles of the superfluid critical temperatures Tc(ρ ) .
Cooling of neutron stars ( NSs ) with the cores composed of neutrons , protons , and electrons is simulated assuming S0 pairing of neutrons in the NS crust , and also S0 pairing of protons and weak P2 pairing of neutrons in the NS core , and using realistic density profiles of the superfluid critical temperatures Tc(ρ ) .
Cooling of neutron stars ( NSs ) with the cores composed of neutrons , protons , and electrons is simulated assuming S0 pairing of neutrons in the NS crust , and also S0 pairing of protons and weak P2 pairing of neutrons in the NS core , and using realistic density profiles of the superfluid critical temperatures Tc(ρ ) .
NeutronsNo subtypeProtons
Cooling of neutron stars ( NSs ) with the cores composed of neutrons , protons , and electrons is simulated assuming S0 pairing of neutrons in the NS crust , and also S0 pairing of protons and weak P2 pairing of neutrons in the NS core , and using realistic density profiles of the superfluid critical temperatures Tc(ρ ) .
Cooling of neutron stars ( NSs ) with the cores composed of neutrons , protons , and electrons is simulated assuming S0 pairing of neutrons in the NS crust , and also S0 pairing of protons and weak P2 pairing of neutrons in the NS core , and using realistic density profiles of the superfluid critical temperatures Tc(ρ ) .
Cooling of neutron stars ( NSs ) with the cores composed of neutrons , protons , and electrons is simulated assuming S0 pairing of neutrons in the NS crust , and also S0 pairing of protons and weak P2 pairing of neutrons in the NS core , and using realistic density profiles of the superfluid critical temperatures Tc(ρ ) .
Cooling of neutron stars ( NSs ) with the cores composed of neutrons , protons , and electrons is simulated assuming S0 pairing of neutrons in the NS crust , and also S0 pairing of protons and weak P2 pairing of neutrons in the NS core , and using realistic density profiles of the superfluid critical temperatures Tc(ρ ) .
Cooling of neutron stars ( NSs ) with the cores composed of neutrons , protons , and electrons is simulated assuming S0 pairing of neutrons in the NS crust , and also S0 pairing of protons and weak P2 pairing of neutrons in the NS core , and using realistic density profiles of the superfluid critical temperatures Tc(ρ ) .
Cooling of neutron stars ( NSs ) with the cores composed of neutrons , protons , and electrons is simulated assuming S0 pairing of neutrons in the NS crust , and also S0 pairing of protons and weak P2 pairing of neutrons in the NS core , and using realistic density profiles of the superfluid critical temperatures Tc(ρ ) .
Cooling of neutron stars ( NSs ) with the cores composed of neutrons , protons , and electrons is simulated assuming S0 pairing of neutrons in the NS crust , and also S0 pairing of protons and weak P2 pairing of neutrons in the NS core , and using realistic density profiles of the superfluid critical temperatures Tc(ρ ) .
Cooling of neutron stars ( NSs ) with the cores composed of neutrons , protons , and electrons is simulated assuming S0 pairing of neutrons in the NS crust , and also S0 pairing of protons and weak P2 pairing of neutrons in the NS core , and using realistic density profiles of the superfluid critical temperatures Tc(ρ ) .
ProtonsNo subtypeNeutrons
Cooling of neutron stars ( NSs ) with the cores composed of neutrons , protons , and electrons is simulated assuming S0 pairing of neutrons in the NS crust , and also S0 pairing of protons and weak P2 pairing of neutrons in the NS core , and using realistic density profiles of the superfluid critical temperatures Tc(ρ ) .
Cooling of neutron stars ( NSs ) with the cores composed of neutrons , protons , and electrons is simulated assuming S0 pairing of neutrons in the NS crust , and also S0 pairing of protons and weak P2 pairing of neutrons in the NS core , and using realistic density profiles of the superfluid critical temperatures Tc(ρ ) .
Cooling of neutron stars ( NSs ) with the cores composed of neutrons , protons , and electrons is simulated assuming S0 pairing of neutrons in the NS crust , and also S0 pairing of protons and weak P2 pairing of neutrons in the NS core , and using realistic density profiles of the superfluid critical temperatures Tc(ρ ) .
Cooling of neutron stars ( NSs ) with the cores composed of neutrons , protons , and electrons is simulated assuming S0 pairing of neutrons in the NS crust , and also S0 pairing of protons and weak P2 pairing of neutrons in the NS core , and using realistic density profiles of the superfluid critical temperatures Tc(ρ ) .
Cooling of neutron stars ( NSs ) with the cores composed of neutrons , protons , and electrons is simulated assuming S0 pairing of neutrons in the NS crust , and also S0 pairing of protons and weak P2 pairing of neutrons in the NS core , and using realistic density profiles of the superfluid critical temperatures Tc(ρ ) .
Cooling of neutron stars ( NSs ) with the cores composed of neutrons , protons , and electrons is simulated assuming S0 pairing of neutrons in the NS crust , and also S0 pairing of protons and weak P2 pairing of neutrons in the NS core , and using realistic density profiles of the superfluid critical temperatures Tc(ρ ) .
Cooling of neutron stars ( NSs ) with the cores composed of neutrons , protons , and electrons is simulated assuming S0 pairing of neutrons in the NS crust , and also S0 pairing of protons and weak P2 pairing of neutrons in the NS core , and using realistic density profiles of the superfluid critical temperatures Tc(ρ ) .
Cooling of neutron stars ( NSs ) with the cores composed of neutrons , protons , and electrons is simulated assuming S0 pairing of neutrons in the NS crust , and also S0 pairing of protons and weak P2 pairing of neutrons in the NS core , and using realistic density profiles of the superfluid critical temperatures Tc(ρ ) .
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