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The composition of the neutron star core for neutrino free matter, without (solid lines) and with (dashed lines) hyperons, for = 5 MeV (upper panel) and = 50 MeV (lower panel).
Source publication
The FSU2H equation of state model, originally developed to describe cold neutron star matter with hyperonic cores, is extended to finite temperature. Results are presented for a wide range of temperatures and lepton fractions, which cover the conditions met in protoneutron star matter, neutron star mergers and supernova explosions. It is found that...
Contexts in source publication
Context 1
... this subsection we show the composition of the star for the abovementioned different cases. In Figure 1 the composition of a neutrino free neutron star core is shown for temperatures = 5 MeV (upper panel) and = 50 MeV (lower panel). The different colors in the figures represent the relative abundance of the particles considered as function of the baryonic density . ...
Context 2
... free case. Every drop of the hyperonic curves corresponds to an appearance of a new hyperon species into the star core. This is particularly visible at the lowest shown temperature of = 10, because the onset of hyperons is more abrupt. Note that, in the neutrino-free = 10 case, three hyperonic species appear at a very similar density (see Fig. 1) and this is visualized as a single drop in the corresponding thermal index curve. At higher temperatures the hyperons are already present at the lower densities in the core, so the thermal index has a smoother behaviour. We can also see that at higher lepton fractions ( = 0.4), as matter is more isospin symmetric, the chemical ...
Context 3
... this subsection we show the composition of the star for the abovementioned different cases. In Figure 1 the composition of a neutrino free neutron star core is shown for temperatures = 5 MeV (upper panel) and = 50 MeV (lower panel). The different colors in the figures represent the relative abundance of the particles considered as function of the baryonic density . ...
Context 4
... free case. Every drop of the hyperonic curves corresponds to an appearance of a new hyperon species into the star core. This is particularly visible at the lowest shown temperature of = 10, because the onset of hyperons is more abrupt. Note that, in the neutrino-free = 10 case, three hyperonic species appear at a very similar density (see Fig. 1) and this is visualized as a single drop in the corresponding thermal index curve. At higher temperatures the hyperons are already present at the lower densities in the core, so the thermal index has a smoother behaviour. We can also see that at higher lepton fractions ( = 0.4), as matter is more isospin symmetric, the chemical ...
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