2007/08/15 by E. M. Kantor, M. E. Gusakov · 4 citations
Physics and Astronomy · #Cosmology and Gravitation Theories #Neutrino Physics Research #Pulsars and Gravitational Waves Research #astro-ph
paper · pdf · doi:10.1111/j.1365-2966.2007.12342.x
published as Mon.Not.Roy.Astron.Soc. 381 (2007) 1702-1710 · 19 pages, 3 figures, accepted for publication in MNRAS
arxiv created 2007/08/15 · openalex publication_date 2007/10/08 · arxiv updated 2009/12/01 · openalex created_date 2016/06/24 · openalex updated_date 2026/07/28
One of the effective mechanisms of neutrino energy losses in red giants, pre‐supernovae and in the cores of white dwarfs is the emission of neutrino–antineutrino pairs in the process of plasmon decay. In this paper, we numerically calculate the emissivity due to plasmon decay in a wide range of temperatures 107–1011 K and densities (2 × 102–1014) g cm−3. Numerical results are approximated by convenient analytical expressions. We also calculate and approximate by analytical expressions the neutrino luminosity of white dwarfs due to plasmon decay, as a function of their mass and internal temperature. This neutrino luminosity depends on the chemical composition of white dwarfs only through the parameter μe (the net number of baryons per electron) and is the dominant neutrino luminosity in all white dwarfs at the neutrino cooling stage.