Energetics of Electron and Ion Acceleration in RHESSI Flares

Details Energetics of Electron and Ion Acceleration in RHESSI Flares Energetics of Electron and Ion Acceleration in RHESSI Flares

Jun 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006spd....37.0128s&link_type=abstract

American Astronomical Society, SPD meeting #37, #1.28; Bulletin of the American Astronomical Society, Vol. 38, p.220

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The Reuven Ramaty High-Energy Solar Spectroscopic Imager (RHESSI) has observed both high-energy electron bremsstrahlung emission and nuclear gamma-ray line emission from solar flares. The gamma-ray lines are produced when energetic ions interact with the ambient medium through various processes including neutron capture and nuclear de-excitation. By comparing electron-related emission and ion-related emission in flares, one can put constraints on the acceleration mechanisms for electrons and ions. Of the gamma-ray lines, RHESSI is most sensitive to the neutron-capture line at 2.223 MeV, which is indirectly produced by protons accelerated above 30 MeV. RHESSI has observed eleven flares with significant neutron-capture line emission and can place upper limits on other flares. We compare the fluence in this line with the electron bremsstrahlung fluence above 300 keV for all RHESSI flares that extend to such energies and find a striking linear correlation between these two quantities across many orders of magnitude in fluence. This correlation implies that the mechanism that accelerates protons above 30 MeV is directly associated with the mechanism that accelerates electrons above 300 keV. On the other hand, we find only a weak correlation between neutron-capture line emission and soft X-ray emission as defined by GOES class. We also find that the correlation of the high-energy populations agrees with observations made by the Solar Maximum Mission (SMM) satellite.The work at the University of California, Berkeley, was supported by NASA contract NAS 5-98033.

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