Energy transport and evaporation of weakly interacting particles in the Sun

Details Energy transport and evaporation of weakly interacting particles in the Sun Energy transport and evaporation of weakly interacting particles in the Sun

Aug 1987

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987phrvd..36.1080n&link_type=abstract

Physical Review D (Particles and Fields), Volume 36, Issue 4, 15 August 1987, pp.1080-1087

Physics

17

Scientific paper

The transport of energy and the evaporation rate of conjectured weakly interacting massive particles in the Sun are calculated by simulating their Brownian motion in a model of the Sun. This is an efficient method for the numerical solution of the Boltzmann equation for these particles as a function of their mass and mean free path l. For values of l comparable to or larger than the radius of the Sun we discuss a new approach to the solution of this equation, while for small values of l we apply the Chapman-Enskog expansion to first order to obtain the luminosity function.

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