Neutrino production from the solar atmosphere

Details Neutrino production from the solar atmosphere Neutrino production from the solar atmosphere

Aug 1985

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985icrc....5..446i&link_type=abstract

In NASA. Goddard Space Flight Center 19th Intern. Cosmic Ray Conf., Vol. 5 p 446-449 (SEE N85-34991 23-93)

Computer Science

Cosmic Rays, Neutrinos, Particle Production, Solar Atmosphere, Sun, Diffusion, Muons, Particle Motion

Scientific paper

When the high energy primary cosmic rays enter near the solar surface, they pass through a thick matter but having a low density. If the density and path length satisfy an appropriate condition, the primaries collide with the constituents near the solar sphere (almost protons) and produce pions and kaons, most of which decay into mu plus numu without successive hadron collisions. Muons also decay into NUmu and NUe before reaching the Earth. The neutrino flux of which the producer is matter near the solar surface is computed by solving cascade diffusion equations. The calculated differential flux of muon neutrino at 1 TeV is 1 X 10 to the minus 13 power (GeV. cm square centimeters 2.s.ster)(-1) which is rather difficult to be observed in the present apparatuses or DUMAND.

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