| | |
| | |
Stat |
Members: 3645 Articles: 2'502'364 Articles rated: 2609
23 April 2024 |
|
| | | |
|
Article overview
| |
|
Strong first-order phase transition in a rotating neutron star core and the associated energy release | J. L. Zdunik
; M. Bejger
; P. Haensel
; E. Gourgoulhon
; | Date: |
25 Jul 2007 | Abstract: | We calculate the energy release associated with a strong first-order phase
transition, from normal phase N to an "exotic" superdense phase S, in a
rotating neutron star. Such a phase transition, accompanied by a density jump
rho_N --> rho_S, is characterized by rho_S/rho_N > 3/2(1+P_0/rho_N c^2), where
P_0 is the pressure, at which phase transition occurs. Configurations with
small S-phase cores are then unstable and collapse into stars with large
S-phase cores. The energy release is equal to the difference in mass-energies
between the initial (normal) configuration and the final configuration
containing an S-phase core, total stellar baryon mass and angular momentum
being kept constant. The calculations of the energy release are based on
precise numerical 2-D calculations. Polytropic equations of state (EOSs) as
well as realistic EOS with strong first-order phase transition due to kaon
condensation are used. For polytropic EOSs, a large parameter space is studied.
For a fixed "overpressure", dP, defined as the relative excess of central
pressure of collapsing metastable star over the pressure of equilibrium
first-order phase transition, the energy release E_rel does not depend on the
stellar angular momentum. It coincides with that for nonrotating stars with the
same dP. Therefore, results of 1-D calculations of E_rel(dP) for non-rotating
stars can be used to predict, with very high precision, the outcome of much
harder to perform 2-D calculations for rotating stars with the same dP. This
result holds also for dP_min < dP < 0, corresponding to phase transitions with
climbing over the energy barrier separating metastable N-phase configurations
from those with an S-phase core. Such phase transitions could be realized in
the cores of newly born, hot, pulsating neutron stars. | Source: | arXiv, 0707.3691 | Services: | Forum | Review | PDF | Favorites |
|
|
No review found.
Did you like this article?
Note: answers to reviews or questions about the article must be posted in the forum section.
Authors are not allowed to review their own article. They can use the forum section.
browser Mozilla/5.0 AppleWebKit/537.36 (KHTML, like Gecko; compatible; ClaudeBot/1.0; +claudebot@anthropic.com)
|
| |
|
|
|
| News, job offers and information for researchers and scientists:
| |