Stabilization of spherically symmetric static Boson stars by Coleman-Weinberg self-interaction potential
arXiv:2402.00061 · doi:10.1016/j.nuclphysb.2024.116764
Abstract
Our motivation in this work is due to the great importance of relativistic boson stars as fierce competitors of black holes. From theoretical perspective, they described by complex Klein Gordon (KG) scalar fields interacting with curved background in general form. In this work we use the Einstein-Klein Gordon (EKG) scalar tensor gravity in presence of the Coleman-Weinberg (CW) self-interaction potential to study formation of a spherically symmetric boson star and situation of its stability. We choose the CW potential because of its important role in description of cosmic inflation.
arXiv comment24 page, 4 figures, This version is accepted to appear in the Journal of Nuclear physics B 2024
References in corpus (11)
- Testing the nature of dark compact objects: a status report
- Gravastars must have anisotropic pressures
- Boson stars driven to the brink of black hole formation
- Models of rotating boson stars and geodesics around them: new type of orbits
- Chaotic inflation, radiative corrections and precision cosmology
- Compact Stars for Undergraduates
- Cosmological Coleman-Weinberg Potentials and Inflation
- Dynamical system approach to scalar-vector-tensor cosmology
- Magnetostatic boson stars
- Boson and neutron stars with increased density
- On the stability of electrostatics stars with modified non-gauge invariant Einstein-Maxwell gravity