Equation of state of fermions in neutron stars

TL;DR

This paper derives the equation of state for fermions in neutron stars considering temperature, chemical potential, and magnetic field effects, revealing how these factors influence neutron star properties and dynamics.

Contribution

It introduces a comprehensive method to compute the neutron star equation of state incorporating statistical effects and magnetic fields, highlighting their impact on star behavior.

Findings

Pressure depends logarithmically on magnetic field strength in strong fields

Regions with higher magnetic fields have shorter lifetimes

High density and magnetic fields are short-lived compared to low ones

Abstract

Employing both the number density and energy density, the equation of state of fermions for each microscopic region of a neutron star is derived in the presence of various statistical effects. It is computed as functions of temperature (T), chemical potential (\mu) and magnetic field (B) based on the statistical properties and corresponding phases of neutron stars. It is revealed that the measurable properties describing the dynamic behavior of a neutron star are determined by the unusual statistical conditions. It is demonstrated that, in a strong magnetic field (B larger than\mu), the pressure (P) shows a logarithmic dependence on B (P is proportional to logarithm of(\mu/B). It is found that the regions with a higher (lower) magnetic field (density) have a shorter (longer) life time. Moreover, the relationship between the magnetic field and chemical potential confirms that the large magnetic field and high density are short lived as compared to low magnetic field and low density at the same temperature.