Medium effects in cooling of neutron stars and the 3P$_\mathsf{2}$ neutron gap

Abstract

We study the dependence of the cooling of isolated neutron stars on the magnitude of the 3P 2 neutron gap. Our "nuclear medium cooling" scenario favors a suppressed value of the 3P 2 neutron gap.

On Manifestation of In-Medium Effects in Neutron Stars and Heavy-Ion Collisions

“…The results of calculations were confronted to the data [67,[82][83][84][85][86] demonstrating an overall agreement of calculations with the data already without necessity to include the DU channel. An example of such calculations is presented in Figure 11, where the cooling curves are shown being computed with MKVOR EoS [87].…”

Constraints on the Nuclear Eos From Neutron Star Observables

“…83 Without such a suppression of the 3 P 2 gap the hadronic cooling scenario would not fulfill the TA constraint. 84 The possibilities of pion condensation and of other so called exotic processes are included in the calculations for purely hadronic stars but do not occur in the hybrid star calculations since the critical density for pion condensation exceeds that for deconfinement in our case. 75 While the hadronic DU process occurs in the DBHF model EoS for all neutron stars with masses above 1.27 M ⊙ , it is not present at all in the DD-F4 model, see the right panel of Fig.…”

The role of medium modifications for neutrino-pair processes from nucleon-nucleon bremsstrahlung

“…vacuum) OPE -henceforth denoted as FOPE -underestimates the cooling of neutron stars. Based on FOPE important medium modifications at ρ ρ 0 /2 are neglected (this has been discussed in details in Senatorov & Voskresensky, 1987;Blaschke et al, 1995;Schaab et al, 1997;Yakovlev et al, 2001;Hanhart et al, 2001;Blaschke et al, 2004;Yakovlev et al, 2005;Grigorian & Voskresensky, 2005;Page & Reddy, 2006;Blaschke et al, 2012Blaschke et al, , 2013, exploring also the role of medium effects for the charged-current absorption reactions, i.e. the modified Urca processes).…”