1996/08/13 by Georg G. Raffelt, Raffelt, Georg G.
Physics and Astronomy · #Astrophysics (astro-ph) #Astrophysics and Cosmic Phenomena #FOS: Physical sciences #Neutrino Physics Research #Particle physics theoretical and experimental studies #astro-ph
paper · pdf · doi:10.48550/arxiv.astro-ph/9608074
5 pages, including 1 figure. Contribution to the Proceedings of Neutrino 96, Helsinki
arxiv created 1996/08/13 · openalex publication_date 1996/08/13 · arxiv updated 2009/12/01 · openalex created_date 2025/10/10 · openalex updated_date 2026/07/28
In a supernova (SN) core during infall and after collapse, neutrinos are trapped by their interactions with nucleons. For the axial-vector current interactions it is not enough to include static particle-particle correlations. Even the single-nucleon spin autocorrelation reduces the scattering cross section dramatically. Therefore, the dynamical structure of the spin-density structure function has an important impact on neutrino transport in supernovae. At the present time, SN neutrino opacities cannot be calculated to a controlled degree of precision.