dorsal/arxiv
View SchemaNeutrino emission in neutron stars
| Authors | E. N. E. van Dalen, A. E. L. Dieperink, J. A. Tjon |
|---|---|
| Categories | |
| ArXiv ID | nucl-th/0303037 |
| URL | https://arxiv.org/abs/nucl-th/0303037 |
| DOI | 10.1103/PhysRevC.67.065807 |
| Journal | Phys.Rev. C67 (2003) 065807 |
Abstract
Neutrino emissivities in a neutron star are computed for the neutrino bremsstrahlung process. In the first part the electro-weak nucleon-nucleon bremsstrahlung is calculated in free space in terms of a on-shell $T$-matrix using a generalized Low energy theorem. In the second part the emissivities are calculated in terms of the hadronic polarization at the two-loop level. Various medium effects, such as finite particle width, Pauli blocking in the $T$-matrix are considered. Compared to the pioneering work of Friman and Maxwell in terms of (anti-symmetrized) one-pion exchange the resulting emissivity is about a factor 4 smaller at saturation density.
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"abstract": "Neutrino emissivities in a neutron star are computed for the neutrino\nbremsstrahlung process. In the first part the electro-weak nucleon-nucleon\nbremsstrahlung is calculated in free space in terms of a on-shell $T$-matrix\nusing a generalized Low energy theorem. In the second part the emissivities are\ncalculated in terms of the hadronic polarization at the two-loop level. Various\nmedium effects, such as finite particle width, Pauli blocking in the $T$-matrix\nare considered. Compared to the pioneering work of Friman and Maxwell in terms\nof (anti-symmetrized) one-pion exchange the resulting emissivity is about a\nfactor 4 smaller at saturation density.",
"arxiv_id": "nucl-th/0303037",
"authors": [
"E. N. E. van Dalen",
"A. E. L. Dieperink",
"J. A. Tjon"
],
"categories": [
"nucl-th",
"astro-ph"
],
"doi": "10.1103/PhysRevC.67.065807",
"journal_ref": "Phys.Rev. C67 (2003) 065807",
"title": "Neutrino emission in neutron stars",
"url": "https://arxiv.org/abs/nucl-th/0303037"
},
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