A new covariant formulation of radial perturbations for imperfect fluids in GR yields a causality-imposed upper bound on the compactness of stable anisotropic stars.
[58] reads pt−pr =ζHβpr⇔3 2Π =−ζHβ(p+ Π),(A2) whereζH∈Randβ=β(xα)is a function of the spacetime representing the compactness of the star at a given circumferential radius
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Radial adiabatic perturbations of stellar compact objects
A new covariant formulation of radial perturbations for imperfect fluids in GR yields a causality-imposed upper bound on the compactness of stable anisotropic stars.