648 K
9 pp.
View Document 
TitleHelium (3) Rich Solar Flares
Author(s)Colgate, S. A.; Audouze, J.; Fowler, W. A.
Publication DateMay 03, 1977
Report NumberLA-UR-77-1055
Unique IdentifierACC0136
Other NumbersCONF-770808-2; OSTI ID: 7284990
Research OrgLos Alamos Scientific Lab., New Mexico. (USA) [Los Alamos National Laboratory]
Contract NoW-7405-ENG-36
Sponsoring OrgEnergy Research and Development Administration (ERDA)
Other Information15th International Cosmic Ray Conference; Aug 13 - 26, 1977; Provdiv, Bulgaria
Subject640104 -- Astrophysics & Cosmology -- Solar Phenomena; Solar Flares -- Chemical Composition; Confinement; Convection; Currents; Helium; Helium 3; Helium 4; Instability; Magnetic Fields; Plasma; Spallation; Temperature Dependence; X-ray Spectra
KeywordsCryogenic Fluids; Elements; Energy Transfer; Even-even Nuclei; Even-odd Nuclei; Fluids; Heat Transfer; Helium Isotopes; Isotopes; Light Nuclei; Nonmetals; Nuclear Reactions; Nuclei; Rare Gases; Solar Activity; Spectra; Stable Isotopes
Related Web PagesWilliam Fowler and Elements in the Stars
AbstractThe extreme enrichment of {sup 3} He {sup 4} He greater than or equal to 1 in some solar flares as due to spallation and the subsequent confinement of the products in a high temperature, kT approx. = 200 keV, high density, n{sub e} approx. = 3 x 10{sup 15} cm {sup -3} plasma associated with the magnetic instability producing the flare is interpreted. The pinch or filament is a current of high energy protons that creates the spallation and maintains the temperature that produces the high energy x-ray spectrum and depletes other isotopes D, Li, Be, and B as observed. Finally the high temperature plasma is a uniquely efficient spallation target that is powered by the interaction of stellar convection and self generated magnetic field.
648 K
9 pp.
View Document 

Some links on this page may take you to non-federal websites. Their policies may differ from this site.