%0 Journal Article
%T The Particular Lines in the Solar Neutrino Energy Spectrum
%A Boris I. Goryachev
%J Journal of Modern Physics
%P 1519-1523
%@ 2153-120X
%D 2013
%I Scientific Research Publishing
%R 10.4236/jmp.2013.411185
%X <p>
	<span style=\"font-family:Verdana;\">In this paper</span><span style=\"font-family:Verdana;\">,</span><span style=\"font-family:Verdana;\"> much attention is given to lines of minimum
and maximum neutrino energies.</span><span> </span><span style=\"font-family:Verdana;\">Tritium chain of the hydrogen cycle in the Sun including
reactions</span><span><span style=\"font-family:Verdana;\"> of </span><sup><span style=\"font-family:Verdana;\">3</span></sup><span style=\"font-family:Verdana;\">He(e</span><sup><span style=\"font-family:Verdana;\">-</span></sup><span style=\"font-family:Verdana;\">,¦Í</span><sub><span style=\"font-family:Verdana;\">e</span></sub><span style=\"font-family:Verdana;\">)</span><sup><span style=\"font-family:Verdana;\">3</span></sup><span style=\"font-family:Verdana;\">H(p,¦Ã)</span><sup><span style=\"font-family:Verdana;\">4</span></sup></span><span><span style=\"font-family:Verdana;\"> is considered. At the
distance of 1</span><span> </span><span style=\"font-family:Verdana;\">a.u.</span><span style=\"font-family:Verdana;\">,</span><span style=\"font-family:Verdana;\"> the flux of tritium neutrinos is equal to 8.1</span><span> </span><span style=\"font-family:Verdana;\">¡Á</span><span> </span><span><span style=\"font-family:Verdana;\">10</span><span style=\"font-family:Verdana;\"><sup>4</sup></span><span style=\"font-family:Verdana;\"> cm<span style=\"line-height:15px;\"><sup>-2</sup>¡¤</span></span><span style=\"font-family:Verdana;\">s<span style=\"line-height:15px;\"><sup>-1</sup></span></span><span style=\"font-family:Verdana;\">. It is an order of magnitude higher than the
flux of the (hep)-neutrinos. Radial distribution of </span><span style=\"font-family:Verdana;\"><sup>3</sup></span><span style=\"font-family:Verdana;\">H-neutrinos
yield inside the Sun and their energy spectrum which has a form of line at the
energy of</span><span style=\"font-family:Verdana;\"> (2.5</span></span><span style=\"font-family:Verdana;\"> - </span><span style=\"font-family:Verdana;\">3.0) keV are calculated. The flux of
thermal tritium neutrinos is accompanied by a very weak flux of antineutrin</span><span><span style=\"font-family:Verdana;\">os (~10</span><span style=\"font-family:Verdana;\"><sup>3</sup></span></span><span> </span><span><span style=\"font-family:Verdana;\">cm<span style=\"line-height:15px;\"><sup>-2</sup>¡¤</span></span><span style=\"font-family:Verdana;\">year<span style=\"line-height:15px;\"><sup>-1</sup></span></span><span style=\"font-family:Verdana;\">) with energy</span></span><span> </span><span><span
%K Solar Neutrino Fluxes
%K Hydrogen-Cycle Chains
%K Standard Solar Models
%U http://www.scirp.org/journal/PaperInformation.aspx?PaperID=40052