A theory of finite-temperature Bose-Einstein condensates in neutron stars
arXiv:1403.3812 · doi:10.1140/epjd/e2014-50380-3
Abstract
We investigate the possible occurrence of a Bose-Einstein condensed phase of matter within neutron stars due to the formation of Cooper pairs among the superfluid neutrons. To this end we study the condensation of bosonic particles under the influence of both a short-range contact and a long-range gravitational interaction in the framework of a Hartree-Fock theory. We consider a finite-temperature scenario, generalizing existing approaches, and derive macroscopic and astrophysically relevant quantities like a mass limit for neutron stars.
21 pages, 9 figures; replaced after publication with additional comments
References in corpus (7)
- Shapiro delay measurement of a two solar mass neutron star
- A Massive Pulsar in a Compact Relativistic Binary
- Neutron Star Observations: Prognosis for Equation of State Constraints
- Rapid Cooling of the Neutron Star in Cassiopeia A Triggered by Neutron Superfluidity in Dense Matter
- BCS-BEC crossover of neutron pairs in symmetric and asymmetric nuclear matter
- Neutron star equilibrium configurations within a fully relativistic theory with strong, weak, electromagnetic, and gravitational interactions
- Condensate dark matter stars
Cited by in corpus (8)
- Evolution and dynamical properties of Bose-Einstein condensate dark matter stars
- Bosonic dark matter dynamics in hybrid neutron stars
- Bose-Einstein condensation in a rigidly rotating relativistic boson gas
- Rotating Bose-Einstein Condensate Stars at finite temperature
- Magnetized vector boson gas at any temperature
- Magnetized BEC stars with boundary conditions depending on magnetic field
- Constraints on Bose-Einstein condensate stars as neutron stars models from new observational data
- Efectos del campo magnético en un gas de bosones vectoriales neutros: aplicaciones astrofísicas