期刊
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
卷 487, 期 2, 页码 2639-2652出版社
OXFORD UNIV PRESS
DOI: 10.1093/mnras/stz1459
关键词
dense matter; equation of state; stars: neutron
资金
- European COST Actions through STSM grants [MP1304, CA16214]
- Alexander von Humboldt Foundation
- Deutsche Forschungsgemeinschaft [SE 1836/4-1]
- National Science Foundation (USA) [PHY-1714068]
The thermal evolution of hypernuclear compact stars is studied for stellar models constructed on the basis of covariant density functional theory in Hartree and Hartree-Fock approximation. Parametrizations of both types are consistent with the astrophysical mass constraints on compact stars and available hypernuclear data. We discuss the differences of these density functionals and highlight the effects they have on the composition and on the cooling of hypernuclear stars. It is shown that hypernuclear stars computed with density functional models that have a low symmetry energy slope, L, are fairly consistent with the cooling data of observed compact stars. The class of stellar models based on larger L values gives rise to the direct Urca process at low densities, which leads to significantly faster cooling. We conjecture high-density pairing for protons and Lambda's in the P-wave channel and provide simple scaling arguments to obtain these gaps. As a consequence themostmassive stellarmodels with masses 1.8 <= M/M-circle dot <= 2 experience slower cooling by hyperonic dUrca processes which involve Lambda's and protons.
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