English (United Kingdom)

https://curated-unify.zendy.io/wp-json/zendy-region/v1/featured_content/oa?rat=en

https://curated-unify.zendy.io/wp-json/zendy-region/v1/highlighted_journal/

Global: Zendy Tools annual

Presents the keyphrase highlighting as premium feature

Keyphrase Highlighting

Presents the summarisation as premium feature

Summarisation

Insights

Presents the pdf analysis as premium feature

PDF Analysis

Presents the zaia usage as premium feature

ZAIA

Global: Zendy Tools monthly

Global: Zendy Plus monthly

Presents the access of premium content as premium feature

Premium Content

Global: Zendy Plus annual

Global: Zendy Free Plan

We calculate the energy release associated with a strong first-order phasetransition, from normal phase N to an "exotic" superdense phase S, in arotating neutron star. Such a phase transition, accompanied by a density jumprho_N --> rho_S, is characterized by rho_S/rho_N > 3/2(1+P_0/rho_N c^2), whereP_0 is the pressure, at which phase transition occurs. Configurations withsmall S-phase cores are then unstable and collapse into stars with largeS-phase cores. The energy release is equal to the difference in mass-energiesbetween the initial (normal) configuration and the final configurationcontaining an S-phase core, total stellar baryon mass and angular momentumbeing kept constant. The calculations of the energy release are based onprecise numerical 2-D calculations. Polytropic equations of state (EOSs) aswell as realistic EOS with strong first-order phase transition due to kaoncondensation are used. For polytropic EOSs, a large parameter space is studied.For a fixed "overpressure", dP, defined as the relative excess of centralpressure of collapsing metastable star over the pressure of equilibriumfirst-order phase transition, the energy release E_rel does not depend on thestellar angular momentum. It coincides with that for nonrotating stars with thesame dP. Therefore, results of 1-D calculations of E_rel(dP) for non-rotatingstars can be used to predict, with very high precision, the outcome of muchharder to perform 2-D calculations for rotating stars with the same dP. Thisresult holds also for dP_min < dP < 0, corresponding to phase transitions withclimbing over the energy barrier separating metastable N-phase configurationsfrom those with an S-phase core. Such phase transitions could be realized inthe cores of newly born, hot, pulsating neutron stars.

Strong first-order phase transition in a rotating neutron star core and the associated energy release