Bi-metric pseudo-Finslerian spacetimes

Abstract

Finsler spacetimes have become increasingly popular within the theoretical physics community over the last two decades. Because physicists need to use pseudo-Finsler structures to describe propagation}of signals, there will be nonzero null vectors in both the tangent and cotangent spaces --- this causes significant problems in that many of the mathematical results normally obtained for "usual" (Euclidean signature) Finsler structures either do not apply, or require significant modifications to their formulation and/or proof. We shall first provide a few basic definitions, explicitly demonstrating the interpretation of bi-metric theories in terms of pseudo-Finsler norms. We shall then discuss the tricky issues that arise when trying to construct an appropriate pseudo-Finsler metric appropriate to bi-metric spacetimes. Whereas in Euclidian signature the construction of the Finsler metric typically fails at the zero vector, in Lorentzian signature the Finsler metric is typically ill-defined on the entire null cone.

8 pages

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Cited by in corpus (11)

• Classical-physics applications for Finsler $b$ space
• Finsler-Randers Cosmology: dynamical analysis and growth of matter perturbations
• Cyclic and Ekpyrotic Universes in Modified Finsler Osculating Gravity on Tangent Lorentz Bundles
• Weak field equations and generalized FRW cosmology on the tangent Lorentz bundle
• On the analyticity of static solutions of a field equation in Finsler gravity
• Applications of the Schwarzschild-Finsler-Randers model
• Schwarzschild-Finsler-Randers spacetime: Dynamical analysis, Geodesics and Deflection Angle
• The causal structure of spacetime is a parameterized Randers geometry
• Aspects of General Relativity: Pseudo-Finsler extensions, Quasi-normal frequencies and Multiplication of tensorial distributions
• Wind-Finslerian structure of black holes
• A volume element on time orientable Finslerian spacetimes