The Extreme Energies Lines in the Solar Neutrino Spectrum

TL;DR

This paper analyzes the solar neutrino spectrum, focusing on the tritium chain, and predicts specific neutrino fluxes and energy lines, including their distribution and associated antineutrino fluxes, providing detailed theoretical insights.

Contribution

It provides detailed calculations of the tritium neutrino flux, energy spectrum, and distribution within the Sun, including the prediction of a distinct energy line at 2.5-3.0 keV and associated antineutrino fluxes.

Findings

Tritium neutrino flux at 1 AU is 8.1×10^4 cm^(-2)s^(-1).

Energy spectrum shows a line at 2.5-3.0 keV.

Maximum energy neutrinos at 19.8 MeV are estimated.

Abstract

Tritium chain of the hydrogen cycle in the Sun including reactions ^3He(e^-,{\nu}_(e))^(3)H(p,{\gamma})^(4)He is considered. At the distance of 1 a.u. the flux of tritium neutrinos is equal to 8.1\cdot 10^(4) cm^(-2)s^(-1). It is an order of magnitude higher than the flux of the (hep)-neutrinos. Radial distribution of ^(3)H-neutrinos yield inside the Sun and their energy spectrum which has a form of line at the energy of (2,5 {\div} 3,0) keV are calculated. The flux of thermal tritium neutrinos is accompanied by a very weak flux of antineutrinos (~ 10^(3) cm^(-2)year^(-1)) with energy lower than 18,6 keV. These antineutrinos are produced during Urca processes ^3He<=>^3H. The flux of the neutrinos of maximum possible energy (line 19,8 MeV) produced due to the (heep)-reaction (related to the (hep)-process) is estimated