Heavy Ion Acceleration in Solar Flares

Details Heavy Ion Acceleration in Solar Flares Heavy Ion Acceleration in Solar Flares

Jan 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002mwoc.conf..387m&link_type=abstract

Multi-Wavelength Observations of Coronal Structure and Dynamics -- Yohkoh 10th Anniversary Meeting. Proceedings of the conferenc

Physics

4

Scientific paper

We present initial results from a self-consistent simulation of particle acceleration and atmospheric heating during impulsive solar flares. The simulation code consists of two main components, the UAH SDSPAC (Spatially-Dependent Stochastic Particle Acceleration Code) and the NRL DSFTM (Dynamic Solar Flux Tube Model) code, together with an interface that allows these two components to communicate. Particle acceleration occurs via cascading MHD turbulence. MHD turbulence (consisting of an admixture of fast mode and Alfven waves) is generated at large scales in the corona and subsequently cascades through the inertial range and into the dissipation range, where it stochastically accelerates both ambient electrons and protons via transit-time and cyclotron resonance, respectively. Both species are energized from thermal to relativistic energies on subsecond timescales. Some of the energetic particles then escape from the corona and enter the chromosphere, where they thermalize through Coulomb collisions. The heated chromosphere then expands into the corona, where the increased density and temperature greatly affect the efficiency of the acceleration process. The highly nonlinear interaction between the acceleration process and the atmospheric response is described by a combined quasilinear and hydrodynamic simulation, based upon the two previously-employed codes above. This is, to our knowledge, the first simulation that accurately takes into account both the micro- and macro-physics of particle acceleration. We present preliminary results such as spatially-dependent energetic particle distributions and coronal temperatures and densities, and discuss their application to spatially-resolved hard and soft X-ray spectra to be obtained from HESSI. This work is supported by NASA Solar Physics grant NAG5-8480.

Affiliated with

Also associated with

No associations

Rating

Heavy Ion Acceleration in Solar Flares does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.

If you have personal experience with Heavy Ion Acceleration in Solar Flares, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Heavy Ion Acceleration in Solar Flares will most certainly appreciate the feedback.

Rate now

Comments { 0 }

Profile ID: LFWR-SCP-O-1838653