Effect of hypothetical, weakly interacting, massive particles on energy transport in the solar interior

Details Effect of hypothetical, weakly interacting, massive particles on energy transport in the solar interior Effect of hypothetical, weakly interacting, massive particles on energy transport in the solar interior

Jul 1985

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985apj...294..663s&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 294, July 15, 1985, p. 663-673.

Astronomy and Astrophysics

Astrophysics

139

Nuclear Fusion, Particle Interactions, Solar Interior, Solar Neutrinos, Stellar Cores, Angular Momentum, Anisotropy, Energy Transfer, Evaporation, Orbits, Scattering Cross Sections, Weak Interactions (Field Theory)

Scientific paper

An unlikely but possible solution to the solar neutrino problem is discussed. (The solution is unlikely only in requiring the existence in the sun of a stable, neutral particle, with a mass in the range of 5-60 GeV, and with a scattering cross section on protons in the range of 10 to the -26th to 10 to the -46th cm-squared.) With such a mass, the particle will populate only the inner 'solar neutrino unit-producing' core and not the larger luminosity-producing region. If it has scattering cross section on protons of 4 x 10 to the -36th cm-squared, then a fractional abundance of the 10 to the -12th will have order unity effect on the sun's thermal transport, in the direction of decreasing the expected neutrino signature. For smaller cross sections, the required abundance rises in inverse proportion, so that cross sections as small as 10 to the -46th cm-squared are effective if the concentration is as large as about 10 to the minus 2. The photino is a possible candidate particle; mirror neutron is may also be candidates.

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