Deka-KeV X-Ray Emission Associated with the Onset of Radio Noise Storms

Details Deka-KeV X-Ray Emission Associated with the Onset of Radio Noise Storms Deka-KeV X-Ray Emission Associated with the Onset of Radio Noise Storms

Aug 1996

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996soph..167..333c&link_type=abstract

Solar Physics, Volume 167, Issue 1-2, pp. 333-348

Physics

14

Scientific paper

Radio noise storms show that suprathermal electrons (a few tens of keV) are present in the vicinity of active regions during several hours or even a few days. Where and how these electrons are energized is not yet well known. A flare-like sudden energy release in the active region is in general observed at the onset of noise storms, either as a fully developed flare or, more often, as a soft X-ray brightening without conspicuous Hα signature. In order to investigate to what extent electrons energized in the active region contribute to the noise-storm emission in the overlying coronal structures, we combine radio imaging (Nançay radioheliograph) with X-ray spectral observations at photon energies of a few keV (GOES) and - for the first time - around 10 keV (WATCH/GRANAT). In two of four studied events the WATCH data show a significant excess of the deka-keV count rate above the expectation from an isothermal fit to the GOES fluxes. Although the electron population producing the deka-keV X-ray emission would be energetic enough to power the simultaneous radio noise storm, the much longer duration of the radio emission requires time-extended particle acceleration. The acceleration probably occurs in the corona overlying the X-ray emitting region, triggered by the processes which give rise to the X-ray brightenings.

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