The continuous emission of low energy cosmic rays during solar flares

Abstract

A new type of diffusion equation is presented in which the shape of the emission curve and the time during which the emission of energetic flare particles from the solar surface occurs can be prescribed. The diffusion equation utilizes a radially dependent diffusion coefficient in the form of D = Mrβand incorporates the convective and decelerative effects of the solar wind as well as external and internal boundary conditions to the interplanetary diffusion medium. The effect of the continuous emission of energetic solar particles on the intensity curves is shown. The logarithmic curve is utilized as a discriminant in testing for continuous emission and it predicts that in high energy events, the particles are released in an impulsive burst within a few minutes after flare onset. The analysis of solar flare data is shown to be independent of either the convective or decelerative effects of the solar wind. The apparent deviation from the radial diffusion coefficient mode of propagation at very low energies is ascribed to continuous emission. The corresponding solar flare data at slightly higher energies or at different tracking satellite stations all indicate adherence to this mode for electrons as well as for protons. It is postulated that even in the very low energy range, the radial mode prevails. On the basis of the accumulated data from twenty six solar flares studied todate, it is asserted that the radial diffusion coefficient model is the basic mode by which solar flare particles propagate through interplanetary space.