(Self-)Magnetized Bose-Einstein Condensate stars. (arXiv:1812.07657v1 [astro-ph.HE])
<a href="http://arxiv.org/find/astro-ph/1/au:+Angulo_G/0/1/0/all/0/1">G. Quintero Angulo</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Martinez_A/0/1/0/all/0/1">A. Pérez Martínez</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Rojas_H/0/1/0/all/0/1">H. Pérez Rojas</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Paret_D/0/1/0/all/0/1">D. Manreza Paret</a>
We study magnetic field effects on the Equations of State (EoS) and the
structure of Bose-Einstein Condensate (BEC) stars, i.e. a compact object
composed by a gas of interacting spin one bosons formed up by the pairing of
two neutrons. To include the magnetic field in the thermodynamic description,
we suppose that particle-magnetic field and particle-particle interactions are
independent. We consider two configurations for the magnetic field: one where
it constant and externally fixed, and another where it is produced by the
bosons by self-magnetization. Since the magnetic field produces the splitting
of pressures in the directions along and perpendicular to the magnetic axis,
stable configurations of self-magnetized and magnetized BEC stars are studied
using the recently found $gamma$-structure equations that describe axially
symmetric objects. The magnetized BEC stars are, in general spheroidal, less
massive and smaller than the non-magnetic ones, being these effects more
relevant at low densities. For the self-magnetized BEC stars their inner
profiles of magnetic field can be computed as a function of the equatorial
radii. The values obtained for the core and surface magnetic fields are in
agreement with those typical of compact objects.
We study magnetic field effects on the Equations of State (EoS) and the
structure of Bose-Einstein Condensate (BEC) stars, i.e. a compact object
composed by a gas of interacting spin one bosons formed up by the pairing of
two neutrons. To include the magnetic field in the thermodynamic description,
we suppose that particle-magnetic field and particle-particle interactions are
independent. We consider two configurations for the magnetic field: one where
it constant and externally fixed, and another where it is produced by the
bosons by self-magnetization. Since the magnetic field produces the splitting
of pressures in the directions along and perpendicular to the magnetic axis,
stable configurations of self-magnetized and magnetized BEC stars are studied
using the recently found $gamma$-structure equations that describe axially
symmetric objects. The magnetized BEC stars are, in general spheroidal, less
massive and smaller than the non-magnetic ones, being these effects more
relevant at low densities. For the self-magnetized BEC stars their inner
profiles of magnetic field can be computed as a function of the equatorial
radii. The values obtained for the core and surface magnetic fields are in
agreement with those typical of compact objects.
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