dorsal/arxiv
View SchemaMuons and emissivities of neutrinos in neutron star cores
| Authors | O. Elgaroy, L. Engvik, E. Osnes, F. V. De Blasio, M. Hjorth-Jensen, G. Lazzari |
|---|---|
| Categories | |
| ArXiv ID | nucl-th/9510045 |
| URL | https://arxiv.org/abs/nucl-th/9510045 |
| DOI | 10.1103/PhysRevLett.76.1994 |
| Journal | Phys.Rev.Lett. 76 (1996) 1994-1997 |
Abstract
In this work we consider the role of muons in various URCA processes relevant for neutrino emissions in the core region of neutron stars. The calculations are done for $\beta$--stable nuclear matter with and without muons. We find muons to appear at densities $\rho = 0.15$ fm$^{-3}$, slightly around the saturation density for nuclear matter $\rho_0 =0.16$ fm$^{-3}$. The direct URCA processes for nucleons are forbidden for densities below $\rho = 0.5$ fm$^{-3}$, however the modified URCA processes with muons $(n+N\rightarrow p+N +\mu +\overline{\nu}_{\mu}, p+N+\mu \rightarrow n+N+\nu_{\mu}$), where $N$ is a nucleon, result in neutrino emissivities comparable to those from $(n+N\rightarrow p+N +e +\overline{\nu}_e, p+N+e \rightarrow n+N+\nu_e$). This opens up for further possibilities to explain the rapid cooling of neutrons stars. Superconducting protons reduce however these emissivities at densities below $0.4$ fm$^{-3}$.
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"abstract": "In this work we consider the role of muons in various URCA processes relevant\nfor neutrino emissions in the core region of neutron stars. The calculations\nare done for $\\beta$--stable nuclear matter with and without muons. We find\nmuons to appear at densities $\\rho = 0.15$ fm$^{-3}$, slightly around the\nsaturation density for nuclear matter $\\rho_0 =0.16$ fm$^{-3}$. The direct URCA\nprocesses for nucleons are forbidden for densities below $\\rho = 0.5$\nfm$^{-3}$, however the modified URCA processes with muons $(n+N\\rightarrow p+N\n+\\mu +\\overline{\\nu}_{\\mu}, p+N+\\mu \\rightarrow n+N+\\nu_{\\mu}$), where $N$ is a\nnucleon, result in neutrino emissivities comparable to those from\n$(n+N\\rightarrow p+N +e +\\overline{\\nu}_e, p+N+e \\rightarrow n+N+\\nu_e$). This\nopens up for further possibilities to explain the rapid cooling of neutrons\nstars. Superconducting protons reduce however these emissivities at densities\nbelow $0.4$ fm$^{-3}$.",
"arxiv_id": "nucl-th/9510045",
"authors": [
"O. Elgaroy",
"L. Engvik",
"E. Osnes",
"F. V. De Blasio",
"M. Hjorth-Jensen",
"G. Lazzari"
],
"categories": [
"nucl-th"
],
"doi": "10.1103/PhysRevLett.76.1994",
"journal_ref": "Phys.Rev.Lett. 76 (1996) 1994-1997",
"title": "Muons and emissivities of neutrinos in neutron star cores",
"url": "https://arxiv.org/abs/nucl-th/9510045"
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