dorsal/arxiv
View SchemaDirect Urca neutrino radiation from superfluid baryonic matter
| Authors | Armen Sedrakian |
|---|---|
| Categories | |
| ArXiv ID | nucl-th/0411061 |
| URL | https://arxiv.org/abs/nucl-th/0411061 |
| DOI | 10.1016/j.physletb.2004.12.026 |
| Journal | Phys.Lett. B607 (2005) 27-34 |
Abstract
Dense matter in compact stars cools efficiently by neutrino emission via the direct Urca processes n -> p + e + nu and p + e -> n + nu. Below the pairing phase transition temperature Tc these processes are suppressed - at asymptotically low temperatures exponentially. We compute the emissivity of the Urca process at one loop for temperatures T < Tc, in the case where the baryons are paired in the 1S0 partial wave. The Urca process is suppressed linearly, rather than exponentially, within the temperature range 0.1 < T/Tc < 1. The charge-current Cooper pair-breaking process contributes up to 50% of the total Urca emissivity in this temperature range.
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"abstract": "Dense matter in compact stars cools efficiently by neutrino emission via the\ndirect Urca processes n -\u003e p + e + nu and p + e -\u003e n + nu. Below the pairing\nphase transition temperature Tc these processes are suppressed - at\nasymptotically low temperatures exponentially. We compute the emissivity of the\nUrca process at one loop for temperatures T \u003c Tc, in the case where the baryons\nare paired in the 1S0 partial wave. The Urca process is suppressed linearly,\nrather than exponentially, within the temperature range 0.1 \u003c T/Tc \u003c 1. The\ncharge-current Cooper pair-breaking process contributes up to 50% of the total\nUrca emissivity in this temperature range.",
"arxiv_id": "nucl-th/0411061",
"authors": [
"Armen Sedrakian"
],
"categories": [
"nucl-th",
"astro-ph"
],
"doi": "10.1016/j.physletb.2004.12.026",
"journal_ref": "Phys.Lett. B607 (2005) 27-34",
"title": "Direct Urca neutrino radiation from superfluid baryonic matter",
"url": "https://arxiv.org/abs/nucl-th/0411061"
},
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