Observables of spheroidal magnetized Strange Stars. (arXiv:2010.06514v1 [astro-ph.HE])
<a href="http://arxiv.org/find/astro-ph/1/au:+Terrero_D/0/1/0/all/0/1">Diana Alvear Terrero</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Perez_S/0/1/0/all/0/1">Samantha López Pérez</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Paret_D/0/1/0/all/0/1">Daryel Manreza Paret</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Martinez_A/0/1/0/all/0/1">Aurora Pérez Martínez</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Angulo_G/0/1/0/all/0/1">Gretel Quintero Angulo</a>
We study stable spheroidal configurations of magnetized Strange Stars using
an axially symmetric metric in spherical coordinates that uses a gamma
parameter to link the anisotropy in the Equation of State due to the magnetic
field with the deformation of the star. The stars are composed by magnetized
Strange Quark Matter described within the framework of the MIT-Bag model. Their
masses, radii, eccentricity, redshift and mass quadrupole moment are computed.
Results are compared with spherical Strange Stars solutions obtained with TOV
equations and observational data of Strange Stars candidates. In the spheroidal
model the observables depend directly on the deformation of the stars, and even
though it is small, the observables strongly deviate from the corresponding
spherical configurations. Thus, the highest values of the mass quadrupole
moment correspond to the intermediate mass regime. These differences might
allow to discriminate between models with/without magnetic field when compared
with observations.
We study stable spheroidal configurations of magnetized Strange Stars using
an axially symmetric metric in spherical coordinates that uses a gamma
parameter to link the anisotropy in the Equation of State due to the magnetic
field with the deformation of the star. The stars are composed by magnetized
Strange Quark Matter described within the framework of the MIT-Bag model. Their
masses, radii, eccentricity, redshift and mass quadrupole moment are computed.
Results are compared with spherical Strange Stars solutions obtained with TOV
equations and observational data of Strange Stars candidates. In the spheroidal
model the observables depend directly on the deformation of the stars, and even
though it is small, the observables strongly deviate from the corresponding
spherical configurations. Thus, the highest values of the mass quadrupole
moment correspond to the intermediate mass regime. These differences might
allow to discriminate between models with/without magnetic field when compared
with observations.
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