Chameleon stars

Abstract

We consider a gravitating spherically symmetric configuration consisting of a scalar field non-minimally coupled to ordinary matter in the form of a perfect fluid. For this system we find static, regular, asymptotically flat solutions for both relativistic and non-relativistic cases. It is shown that the presence of the non-minimal interaction leads to substantial changes both in the radial matter distribution of the star and in the star's total mass. A simple stability test indicates that, for the choice of parameters used in the paper, the solutions are unstable.

final version, to be published in PRD

References in corpus (6)

• Dynamics of dark energy
• Nonminimal coupling of perfect fluids to curvature
• Gravitational Stability of Boson Stars
• A Star Harbouring a Wormhole at its Core
• On the stability of spherically symmetric and wormhole solutions supported by the sine-Gordon ghost scalar field
• Chameleon Cosmology Model Describing the Phantom Divide Line Crossing

Cited by in corpus (19)

• Dynamical Boson Stars
• Physically viable solutions of anisotropic spheres in $f(\mathcal{R},\mathcal{G})$ gravity satisfying the Karmarkar condition
• Boson Stars and Oscillatons: A Review
• On charged boson stars
• A study of anisotropic spheres in $f(Q)$ gravity with quintessence field
• Mixed neutron-star-plus-wormhole systems: Linear stability analysis
• Dynamical evolution of dark matter admixed neutron stars
• Mixed neutron-star-plus-wormhole systems: Equilibrium configurations
• Rotating dark matter admixed neutron stars
• A Conjecture on the Minimal Size of Bound States
• Charged Anisotropic Finch-Skea-Bardeen Spheres
• Wormhole solutions supported by interacting dark matter and dark energy
• Relativistic polytropic spheres embedded in a chameleon scalar field
• Fermion-charged-boson stars
• Dynamical evolution of fermion-boson stars with realistic equations of state
• Nonrelativistic isothermal fluid in the presence of a chameleon scalar field: Static and collapsing configurations
• Chameleon stars supported by a cosmological scalar field
• Chameleon dark matter stars
• Quintessence-Chameleon transitions in anisotropic Kiselev model of neutron stars