A vector-supported compact object in modified gravity relaxes dissipatively without oscillatory ringdown because a hidden chiral symmetry converts perturbations into one-way transport.
Relativistic stars in vector-tensor theories
2 Pith papers cite this work. Polarity classification is still indexing.
2
Pith papers citing it
abstract
We study relativistic star solutions in second-order generalized Proca theories characterized by a $U(1)$-breaking vector field with derivative couplings. In the models with cubic and quartic derivative coupling, the mass and radius of stars become larger than those in general relativity for negative derivative coupling constants. This phenomenon is mostly attributed to the increase of star radius induced by a slower decrease of the matter pressure compared to general relativity. There is a tendency that the relativistic star with a smaller mass is not gravitationally bound for a low central density and hence dynamically unstable, but that with a larger mass is gravitationally bound. On the other hand, we show that the intrinsic vector-mode couplings give rise to general relativistic solutions with a trivial field profile, so the mass and radius are not modified from those in general relativity.
fields
gr-qc 2years
2026 2verdicts
UNVERDICTED 2representative citing papers
In scalar-vector-tensor gravity, the vector-curvature coupling alters neutron star mass-radius curves and radial oscillation frequencies while preserving the coincidence of maximum mass with the onset of radial instability.
citing papers explorer
-
Relaxation without ringdown for a compact object in modified gravity
A vector-supported compact object in modified gravity relaxes dissipatively without oscillatory ringdown because a hidden chiral symmetry converts perturbations into one-way transport.
-
Radial Oscillations of Neutron Stars with Vector-Induced Scalar Hair
In scalar-vector-tensor gravity, the vector-curvature coupling alters neutron star mass-radius curves and radial oscillation frequencies while preserving the coincidence of maximum mass with the onset of radial instability.