Interplanetary energetic particles, coronal flares and hard X-ray microflares

Details Interplanetary energetic particles, coronal flares and hard X-ray microflares Interplanetary energetic particles, coronal flares and hard X-ray microflares

Apr 1986

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986sfcp.nasa...98l&link_type=abstract

In NASA. Marshall Space Flight Center Solar Flares and Coronal Physics Using P/OF as a Research Tool p 98-119 (SEE N86-24614

Physics

Charged Particles, Interplanetary Medium, Solar Corona, Solar Flares, Solar X-Rays, Bremsstrahlung, Electrons, Helium, Ions, Pinhole Occulter Facility, Solar Radio Emission

Scientific paper

Solar electron phenomena which can produce low levels of hard X-ray emission at the Sun are reviewed. Small approx. 2 to 100 keV solar electrons events, the most common type of impulsive solar particle emission, appear to originate in flare-like bursts high in the corona. These events often are accompanied by approx. 1 MeV/nucleon to the 3rd power He-rich particle events in which lower energy ions are apparently accelerated as well. Long-lived (many days) streams associated with large flares or interplanetary shocks dominate the interplanetary electron fluxes, but even at the quietest times a significant outflow of non-thermal approx. 2 keV electrons occurs. These electron phenomena are accompanied by coronal and interplanetary radio emission. High sensitivity hard X-ray measurements show that microflares, bursts with peak keV fluxes 10 to 100 times smaller than observed in small solar flares, may occur as often as once every 5 min near solar maximum. The proposed Pinhole/Occulter Facility hard X-ray instrumentation provides the increase in sensitivity required to image these phenomena for the first time.

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