Astronomy and Astrophysics – Astrophysics
Scientific paper
2004-04-02
Astron.Astrophys. 423 (2004) 1063-1072
Astronomy and Astrophysics
Astrophysics
9 pages, 3 figures, submitted to A&A
Scientific paper
10.1051/0004-6361:20041006
We simulate cooling of superfluid neutron stars with nucleon cores where direct Urca process is forbidden. We adopt density dependent critical temperatures $T_{cp}(\rho)$ and $T_{cn}(\rho)$ of singlet-state proton and triplet-state neutron pairing in a stellar core and consider a strong proton pairing (with maximum $T_{cp}^{max} \ga 5 \times 10^9$ K) and a moderate neutron pairing ($T_{cn}^{max} \sim 6 \times 10^8$ K). When the internal stellar temperature $T$ falls below $T_{cn}^{max}$, the neutrino luminosity $L_{CP}$ due to Cooper pairing of neutrons behaves $\propto T^8$, just as that produced by modified Urca process (in a non-superfluid star) but is higher by about two orders of magnitude. In this case the Cooper-pairing neutrino emission acts like an enhanced cooling agent. By tuning the density dependence $T_{cn}(\rho)$ we can explain observations of cooling isolated neutron stars in the scenario in which direct Urca process or similar process in kaon/pion condensed or quark matter are absent.
Gnedin Oleg Yuri
Gusakov Mikhail E.
Kaminker A. D.
Yakovlev Dmitry G.
No associations
LandOfFree
Enhanced cooling of neutron stars via Cooper-pairing neutrino emission does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.
If you have personal experience with Enhanced cooling of neutron stars via Cooper-pairing neutrino emission, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Enhanced cooling of neutron stars via Cooper-pairing neutrino emission will most certainly appreciate the feedback.
Profile ID: LFWR-SCP-O-144559