2000/06/28 by W. C. Haxton, W.C. Haxton, Wei Lin · 20 citations
Physics and Astronomy · #Astrophysics and Cosmic Phenomena #Cosmic neutrino background #Cosmic ray #Dark Matter and Cosmic Phenomena #Electron #Electron neutrino #Flux (metallurgy) #Neutrino #Neutrino Physics Research #Solar core #Solar neutrino #astro-ph #hep-ph #nucl-th
paper · pdf · doi:10.1016/s0370-2693(00)00764-4
published in Physics Letters B 486(3-4), 263-271 (Elsevier BV) · Revtex, 5 figures, 13 pages Typo in Fig 5 label corrected in this replacement
arxiv created 2000/06/28 · openalex publication_date 2000/08/01 · arxiv updated 2009/11/30 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/05
We calculate the thermal flux of low-energy solar neutrinos and antineutrinos of all flavors arising from a variety of neutrino pair processes: Compton production (including plasmon-pole diagrams), neutral current decay of thermally populated nuclear states, plasmon decay, and electron transitions from free to atomic bound states. The resulting flux density per flavor is significant (10E8-10E9/cm2/sec/MeV) below about 5 keV, and the distributions fill much of the valley between the high-energy edge of the cosmic background neutrino spectrum and the low energy tails of the pp-chain electron neutrino and terrestrial electron antineutrino spectra. Thermal neutrinos carry information on the solar core temperature distribution and on heavy flavor masses in the range of 1 keV. The detection of these neutrinos is a daunting but interesting challenge.