Other
Scientific paper
May 2006
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006agusmsh41a..01l&link_type=abstract
American Geophysical Union, Fall Meeting 2007, abstract #SH41A-01
Other
7513 Coronal Mass Ejections (2101), 7514 Energetic Particles (2114), 7519 Flares, 7554 X-Rays, Gamma Rays, And Neutrinos, 7984 Space Radiation Environment
Scientific paper
The RHESSI (Ramaty High Energy Solar Spectroscopic Imager) mission detects solar flare hard X-ray/gamma- ray bremsstrahlung continuum and gamma-ray line emissions produced by energetic electrons and ions, respectively, colliding with the solar atmosphere. I review here the comparisons of the timing, location, and spectra of energetic electrons and ions at the Sun, inferred from the RHESSI observations; with the timing, location and spectra of energetic electrons and ions in impulsive and gradual SEP events directly observed in situ near 1 AU by Wind, ACE, and other near-earth spacecraft. Generally, scattering of the SEPs in their interplanetary propagation to 1 AU produces a diffusive time profile that masks the acceleration/injection near the Sun. A few impulsive events exhibit nearly scatter -free propagation (especially for electrons) so they can be accurately traced back to the Sun. These events show two electron injections, one for the <~1 - 10 keV electrons, early enough to produce the type III solar radio burst; and a second injection for >~10-15 keV electrons about ten minutes later. Energetic ions in these impulsive events appear to be injected even later. These impulsive events often lack a flare, but appear to be related to small, >~600km/s coronal mass ejections.
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