Abstract
Exploiting a stiff equation of state of the relativistic mean-field model MKVORH ϕ with σ -scaled hadron effective masses and couplings, including hyperons, we demonstrate that the existing neutron-star cooling data can be appropriately described within “the nuclear medium cooling scenario” under the assumption that different sources have different masses.
Highlights
The equation of state (EoS) of the neutron-star matter should be stiff, cf. [1,2], in order to describe measured masses of the heaviest known pulsars PSR J1614-2230 [3]and PSR J0348+0432 [4]
We demonstrate how a satisfactory explanation of all existing observational data for the temperature–age relation is reached within the “nuclear medium cooling” scenario [11], with the relativistic mean-field (RMF) EoS MKVORHφ with σ-scaled hadron effective masses and coupling constants, including hyperons [7,8]
Which results in a decrease of the maximum neutron-star mass below the observed limit
Summary
The equation of state (EoS) of the neutron-star matter should be stiff, cf [1,2], in order to describe measured masses of the heaviest known pulsars PSR J1614-2230 (of mass M = 1.928 ± 0.017M ) [3]. Within RMF, EoSs with σ-scaled hadron effective masses and coupling constants, the maximum neutron-star mass remains above 2M even when hyperons are included [7,8]. We demonstrate how a satisfactory explanation of all existing observational data for the temperature–age relation is reached within the “nuclear medium cooling” scenario [11], with the RMF EoS MKVORHφ with σ-scaled hadron effective masses and coupling constants, including hyperons [7,8]
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