Relativistic Gravitational Collapse by Thermal Mass
arXiv:2009.11919 · doi:10.1088/1572-9494/abc3ae
Abstract
Gravity and thermal energy are universal phenomena which compete over the stabilization of astrophysical systems. The former induces an inward pressure driving collapse and the latter a stabilizing outward pressure generated by random motion and energy dispersion. Since a contracting self-gravitating system is heated up one may wonder why is gravitational collapse not halted in all cases at a sufficient high temperature establishing either a gravo-thermal equilibrium or explosion. Here, based on the equivalence between mass and energy, we show that there always exists a temperature threshold beyond which the gravitation of thermal energy overcomes its stabilizing pressure and the system collapses under the weight of its own heat.
References in corpus (12)
- From hadrons to quarks in neutron stars: a review
- Perspectives on Core-Collapse Supernova Theory
- Interacting quark matter equation of state for compact stars
- Thermodynamical instabilities of perfect fluid spheres in General Relativity
- The Deconfinement Phase Transition in Proto-Neutron-Star Matter
- Effects of quark matter nucleation on the evolution of proto-neutron stars
- Critical spectrum of fluctuations for deconfinement at proto-neutron star cores
- Relativistic Gravothermal Instabilities
- Corrigendum to "Thermodynamical instabilities of perfect fluid spheres in General Relativity"
- Thermal Mass limit of Neutron Cores
- Gravitational instability caused by the weight of heat
- Signatures of QCD Phase Transition in a Newborn Compact Star