Abstract
We investigate the physical properties of the protoneutron stars in the framework of a relativistic mean-field theory based on nonextensive statistical mechanics, characterized by power-law distributions. We study the finite-temperature equation of state in, β-stable matter at fixed entropy per baryon, in the absence and in the presence of hyperons and trapped neutrinos. We show that nonextensive power-law effects could play a crucial role in the structure and in the evolution of the protoneutron stars also for small deviations from the standard Boltzmann-Gibbs statistics.
Highlights
A protoneutron star (PNS) is formed in a stellar remnant after a successful core-collapse supernova explosion of a star with a mass smaller than about 20 solar masses and in the first seconds of its evolution it is a very hot, lepton rich and β-stable object and a lepton concentration typical of the pre-supernova matter [1].The essential microphysical ingredients that govern the macrophysical evolution of the PNS in the so-called Kelvin-Helmholtz epoch, during which the remnant changes from a hot and lepton-rich PNS to a cold and deleptonized neutron star, are the equation of state EOS of dense matter and its associated neutrino opacity
The PNS is in quasi-stationary β-equilibrium state during its evolution because the time scale of the weak interaction is much shorter than the time scale of neutrino diffusion
The knowledge of the nuclear EOS of dense matter at finite temperature plays a crucial role in the determination of the structure and in the macrophysical evolution of the PNS [2, 3]
Summary
This content has been downloaded from IOPscience. Please scroll down to see the full text. Ser. 665 012071 (http://iopscience.iop.org/1742-6596/665/1/012071) View the table of contents for this issue, or go to the journal homepage for more. Download details: IP Address: 193.205.65.86 This content was downloaded on 09/02/2016 at 13:34 Please note that terms and conditions apply
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