  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.
