Magnetic tension and gravitational collapse

Tsagas, Christos G.

doi:10.1088/0264-9381/23/13/002

Cited by 26 publications

(55 citation statements)

References 35 publications

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“…‡‡ ‡‡This brings in mind the ideal Magnetohydrodynamics (MHD) limit where the Riemannian curvature is non‐trivially involved in the expansion dynamics through a magnetocurvature coupling. There, the Weyl curvature also enters the Raychaudhuri's equation . Similarities are expected since from relation Finsler–Randers geodesics can be physically interpreted as magnetic flows on a Riemannian manifold.…”

mentioning

confidence: 56%

Relativistic Finsler geometry

Kouretsis

Stathakopoulos

Stavrinos

2013

Math Methods in App Sciences

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We briefly review some basic concepts of parallel displacement in Finsler geometry. In general relativity, the parallel translation of objects along the congruence of the fundamental observer corresponds to the evolution in time. By dropping the quadratic restriction on the measurement of an infinitesimal distance, the geometry is generalized to a Finsler structure. Apart from curvature a new property of the manifold complicates the geometrodynamics, the color. The color brings forth an intrinsic local anisotropy and many quantities depend on position and to a "supporting" direction. We discuss this direction dependence and some physical interpretations. Also, we highlight that in Finsler geometry the parallel displacement isn't necessarily always along the "supporting" direction. The latter is a fundamental congruence of the manifold and induces a natural 1+3 decomposition. Its internal deformation is given through the evolution of the irreducible components of vorticity, shear and expansion.Comment: references added, Contribution to the proceedings of "Modern Mathematical Methods in Science and Technology 2012 (M3ST2012)", Kalamata, Greece, August, 201

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mentioning

confidence: 56%

Relativistic Finsler geometry

Kouretsis

Stathakopoulos

Stavrinos

2013

Math Methods in App Sciences

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“…In this arena the question of a caustic singularity must be revisited. A characteristic example is the collapse of an ideal MHD fluid where magnetic tension may prevent the formation of a caustic 39 . The present phenomenological model points out that the osculation of a Finsler space to a Riemannian one leads to non-geodesic motion.…”

Section: Discussionmentioning

confidence: 99%

Imperfect fluids, Lorentz violations, and Finsler cosmology

Kouretsis

Stathakopoulos²,

Stavrinos

2010

Phys. Rev. D

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We construct a cosmological toy model based on a Finslerian structure of space-time. In particular, we are interested in a specific Finslerian Lorentz violating theory based on a curved version of Cohen and Glashow's Very Special Relativity. The osculation of a Finslerian manifold to a Riemannian leads to the limit of Relativistic Cosmology, for a specified observer. A modified flat FRW cosmology is produced.The analogue of a zero energy particle unfolds some special properties of the dynamics. The kinematical equations of motion are affected by local anisotropies. Seeds of Lorentz Violations may trigger density inhomogeneities to the cosmological fluid.

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“…This further decelerates the expansion if R < 0, but tends to accelerate it when R is positive. This counter-intuitive behaviour, whichresults from the tension of the field, can have nontrivial and veryunexpected implications for spatially curved magnetic spacetimes [143]- [146].…”

Section: Linear Evolutionmentioning

confidence: 99%

Cosmology with inhomogeneous magnetic fields

Barrow¹,

2007

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We review spacetime dynamics in the presence of large-scale electromagnetic fields and then consider the effects of the magnetic component on perturbations to a spatially homogeneous and isotropic universe. Using covariant techniques, we refine and extend earlier work and provide the magnetohydrodynamic equations that describe inhomogeneous magnetic cosmologies in full general relativity. Specialising this system to perturbed Friedmann-Robertson-Walker models, we examine the effects of the field on the expansion dynamics and on the growth of density inhomogeneities, including non-adiabatic modes. We look at scalar perturbations and obtain analytic solutions for their linear evolution in the radiation, dust and inflationary eras. In the dust case we also calculate the magnetic analogue of the Jeans length. We then consider the evolution of vector perturbations and find that the magnetic presence generally reduces the decay rate of these distortions. Finally, we examine the implications of magnetic fields for the evolution of cosmological gravitational waves. 98.62.En; 98.65.Dx

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Magnetic tension and gravitational collapse

Cited by 26 publications

References 35 publications

Relativistic Finsler geometry

Relativistic Finsler geometry

Imperfect fluids, Lorentz violations, and Finsler cosmology

Cosmology with inhomogeneous magnetic fields

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