Many Aspects of Magnetic Fields in Neutron Stars

Negreiros, Rodrigo; Bernal, C. G.; Dexheimer, V.; Troconis, O.

doi:10.3390/universe4030043

Cited by 12 publications

(11 citation statements)

References 77 publications

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“…Here we just reproduce it without details. Thus from ( 36), ( 29)- (31) and P xx = P yy = P zz = P , P xy = 0, µ = µ 0 = constant, it is evident that such a solution is also conformally flat.…”

Section: A the Incompressible Isotropic Spheroidmentioning

confidence: 96%

Complexity factors for axially symmetric static sources

2019

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A previously found definition of complexity for spherically symmetric fluid distributions [1], is extended to axially symmetric static sources. In this case there are three different complexity factors, defined in terms of three structure scalars obtained from the orthogonal splitting of the Riemann tensor. All these three factors vanish, for what we consider the simplest fluid distribution, i.e a fluid spheroid with isotropic pressure and homogeneous energy density. However, as in the spherically symmetric case, they can also vanish for a variety of configurations, provided the energy density inhomogeneity terms cancel the pressure anisotropic ones in the expressions for the complexity factors. Some exact analytical solutions of this type are found and analyzed. At the light of the obtained results, some conclusions about the correlation (the lack of it) between symmetry and complexity, are put forward.

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Section: A the Incompressible Isotropic Spheroidmentioning

confidence: 96%

Complexity factors for axially symmetric static sources

2019

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“…Considering the magnetizing field B to be constant in time and uniform over the radius of the star, as we do in this paper, is also only an approximation. However, given that the relaxation times of the star's magnetic field decay is of the order of ∼10 3 years [50], our present assumption of a constant magnetic field fits amply within the early stages of the magnetic evolution of the star. Similarly, assuming a slow variation of the magnetic field with distance inside highly magnetized stars as presented, for example, in Ref.…”

Section: Inside a Neutron Starmentioning

confidence: 79%

Spin-1/2 Particles under the Influence of a Uniform Magnetic Field in the Interior Schwarzschild Solution

2021

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The relativistic wave equation for spin-1/2 particles in the interior Schwarzschild solution in the presence of a uniform magnetic field is obtained. The fully relativistic regime is considered, and the energy levels occupied by the particles are derived as functions of the magnetic field, the radius of the massive sphere and the total mass of the latter. As no assumption is made on the relative strengths of the particles’ interaction with the gravitational and magnetic fields, the relevance of our results to the physics of the interior of neutron stars, where both the gravitational and the magnetic fields are very intense, is discussed.

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“…As avenues for further work, one should be able to extend this magnetizing method to more general axially-symmetric geometries as required for realistic magnetars in [15]. These geometries will likely require more general anisotropic fluid interior solutions with axial symmetry as in [39], [40].…”

Section: Discussionmentioning

confidence: 99%