Warm and dense stellar matter under strong magnetic fields

TLDR

The study examines how strong magnetic fields influence the equation of state of warm stellar matter in protoneutron stars. Using a relativistic mean‑field nuclear model with hyperons, the authors analyze neutrino‑free and neutrino‑trapped matter at fixed entropy per baryon under a density‑dependent magnetic field ranging from 10^15 G at the surface to 3×10^18 G at the center. The magnetic field suppresses neutrinos at low densities, preventing a hybrid protoneutron star from collapsing into a low‑mass black hole if the field remains strong, but its decay after cooling could trigger such collapse.

Abstract

We investigate the effects of strong magnetic fields on the equation of state of warm stellar matter as it may occur in a protoneutron star. Both neutrino-free and neutrino-trapped matter at a fixed entropy per baryon are analyzed. A relativistic mean-field nuclear model, including the possibility of hyperon formation, is considered. A density-dependent magnetic field with a magnitude of ${10}^{15}\phantom{\rule{0.28em}{0ex}}\mathrm{G}$ at the surface and not more than $3\ifmmode\times\else\texttimes\fi{}{10}^{18}\phantom{\rule{0.28em}{0ex}}\mathrm{G}$ at the center is considered. The magnetic field gives rise to a neutrino suppression, mainly at low densities, in matter with trapped neutrinos. It is shown that a hybrid protoneutron star will not evolve into a low-mass black hole if the magnetic field is strong enough and the magnetic field does not decay. However, the decay of the magnetic field after cooling may give rise to the formation of a low-mass black hole.