Alfven Turbulence Dissipation in Proton Injection and Acceleration in Solar Flares

Details Alfven Turbulence Dissipation in Proton Injection and Acceleration in Solar Flares Alfven Turbulence Dissipation in Proton Injection and Acceleration in Solar Flares

Jun 1995

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995apj...446..390s&link_type=abstract

Astrophysical Journal v.446, p.390

Astronomy and Astrophysics

Astronomy

3

Acceleration Of Particles, Magnetohydrodynamics: Mhd, Sun: Corona, Sun: Flares, Sun: Particle Emission, Waves

Scientific paper

We consider coronal proton acceleration by a spectrum of parallel-propagating Alfvén waves. Both the nonlinear and linear aspects of this acceleration are included, but the Alfvén wave spectrum and total wave energy density are taken as fixed. The proton distribution is followed in detail numerically. The process of nonlinear Landau damping or beat-wave acceleration acts effectively to pull protons from the bulk to beyond the Alfvén velocity, the threshold for gyroresonant or linear acceleration. The gyroresonant acceleration then accelerates a density of 106 cm-3 of protons beyond 10 MeV as required by the observations. For a Kolmogorov spectrum of equal quantities of left- and right-hand polarized waves, moving in both directions along the magnetic field of energy density 1.8 ergs s-3, this density of more than 10 MeV protons occurs in 3 s; there is no production of more than 10 MeV protons in the first second for an initial temperature of 2.0 × 107 K and density of 5.2 × 190 cm-3. The total energy expended is 100.2 ergs cm-3 and the efficiency is 16.5% to beyond 10 MeV. These results satisfy all existing observations. Within the limitation of a fixed wave spectrum and level, this is the first demonstration that Alfvén wave turbulence alone can without any auxiliary injection, produce all of the proton acceleration required in impulsive solar flares.

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