Volume 416, Number 3, March IV 2004
|Page(s)||991 - 996|
|Section||Stellar structure and evolution|
|Published online||09 March 2004|
Energy release due to antineutrino untrapping and diquark condensation in hot quark star evolution
Fachbereich Physik, Universität Rostock, Universitätsplatz 1, 18051 Rostock, Germany
2 Instituto de Física Rosario, Bv. 27 de febrero 210 bis, 2000 Rosario, Argentina e-mail: email@example.com
3 Bogoliubov Laboratory for Theoretical Physics, JINR Dubna, 141980 Dubna, Russia e-mail: firstname.lastname@example.org
4 Department of Physics, Yerevan State University, Alex Manoogian Str. 1, 375025 Yerevan, Armenia e-mail: email@example.com
Corresponding author: D. Blaschke, firstname.lastname@example.org
Accepted: 6 November 2003
We study the consequences of antineutrino trapping in hot quark matter for quark star configurations with possible diquark condensation. Due to the conditions of charge neutrality and β-equilibrium the flavor asymmetry increases with the number density of trapped antineutrinos. Above a critical value of the antineutrino chemical potential of 30 MeV, diquark condensation is inhibited at low densities and a two-phase structure emerges: a superconducting quark matter core surrounded by a shell of normal quark matter. When the quark star cools below a temperature MeV, the mean free path of antineutrinos becomes larger than the thickness of the normal quark matter shell so that they become suddenly untrapped. By comparing the masses of configurations with the same baryon number we estimate that the release of energy due to the antineutrino untrapping transition can be in the range of 1051–1052 erg.
Key words: dense matter / stars: interiors / stars: evolution / stars: neutron
© ESO, 2004
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