Paper detail

Equation of state of fermions in neutron stars

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 (μ) 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 thanμ), the pressure (P) shows a logarithmic dependence on B (P is proportional to logarithm of(μ/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.