L. L. Lopes, D. P. Menezes
Neutron stars are one of the most exotic objects in the universe and a unique
laboratory to study the nuclear matter above the nuclear saturation density. In
this work, we study the equation of state of the nuclear matter within a
relativistic model subjected to a strong magnetic field. We then apply this EoS
to study and describe some of the physical characteristics of neutron star,
especially the massradius relation and chemical compositions. To study the
influence of a the magnetic field and the hyperons in the stellar interior, we
consider altogether six solutions: three different values of magnetic field to
obtain a weak, a moderate and a strong influence, and two configurations: a
family of neutron stars formed only by protons, electrons and neutrons and a
family formed by protons, electrons, neutrons, muons and hyperons. In all cases
the particles that constitute the neutron star are in ${\beta}$ equilibrium and
zero total net charge. In the end, we see that although a magnetar can reaches
$2.50M_{\bigodot}$, arises a natural explanation of why we do not know pulsars
with masses above $2.0M_{\bigodot}$
View original:
http://arxiv.org/abs/1202.5016
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