The influence of strong magnetic fields on proto-quark stars
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TLDR
In this article, different stages of magnetized quark star evolution incorporating baryon number conservation and using an anisotropic energy momentum tensor were analyzed, and the first stages of the evolution were simulated through the inclusion of trapped neutrinos and fixed entropy per particle, while in the last stage the star was taken to be deleptonized and cold.Abstract:
We analyze different stages of magnetized quark star evolution incorporating baryon number conservation and using an anisotropic energy momentum tensor. The first stages of the evolution are simulated through the inclusion of trapped neutrinos and fixed entropy per particle, while in the last stage the star is taken to be deleptonized and cold. We find that, although strong magnetic fields modify quark star masses, the evolution of isolated stars needs to be constrained by fixed baryon number, which necessarily lowers the possible star masses. Moreover, magnetic field effects, measured by the difference between the parallel and perpendicular pressures, are more pronounced in the beginning of the star evolution, when there is a larger number of charged leptons and up quarks. We also show that having a spatially varying magnetic field allows for larger magnetic fields to be supported.read more
Citations
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Consistent neutron star models with magnetic-field-dependent equations of state
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Inverse magnetic catalysis in Nambu–Jona-Lasinio model beyond mean field
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Pions in magnetic field at finite temperature
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Deformation of a magnetized neutron star
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TL;DR: In this article, the effect of the magnetic field on the mass and shape of a star was studied and the excess mass and change in the equatorial radius of the star due to the non-uniform magnetic field was found to be about 3-4% compared to the spherical solution.
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Magnetic susceptibility of a neutron star crust.
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References
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The Convective Urca Process with Implicit Two-Dimensional Hydrodynamics
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TL;DR: In this paper, the role of convective flux in the thermodymics of the convective Urca neutrino loss process in degenerate, convective, quasi-static, carbon-burning cores was considered.
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TL;DR: In this paper, it was shown that the magnetic field of a neutron star cannot exceed 10−19$ G and the thermodynamic pressure of dense magnetized fermion gas is isotropic.