High Resolution Imaging of Solar Flare Footpoints in White Light and Hard X-rays

Details High Resolution Imaging of Solar Flare Footpoints in White Light and Hard X-rays High Resolution Imaging of Solar Flare Footpoints in White Light and Hard X-rays

May 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009spd....40.1919k&link_type=abstract

American Astronomical Society, SPD meeting #40, #19.19; Bulletin of the American Astronomical Society, Vol. 41, p.850

Astronomy and Astrophysics

Astronomy

Scientific paper

High resolution G-band (430 nm) observations ( 0.2 arcsec) taken by HINODE/SOT and hard X-ray observations (2.3 arcsec) from the Reuven Ramaty High Energy Solar Spectroscopic Imager (RHESSI) are used to study footpoint sources of the December 6, 2006 GOES X9 class solar flare. At both wavelengths, several co-spatial footpoint sources are seen on the flare ribbons that show similar relative intensities. This excellent correlation suggests that the energetic electrons producing the hard X-ray emission are also the source of energy for the white light emission, excluding energetic protons as a possible source. If both emissions indeed come from the same location, the higher resolution G-band observation suggest that the individual hard X-ray sources are unresolved. Using the area from the G-band images, the cold thick target model gives the enormous energy deposition rate of 2e12 erg/s/cm2 for 25 keV (9e12 erg/s/cm2 for 10 keV) and huge densities of beam electrons within the hard X-ray source of 0.3e10 cm-3 above 25 keV (5d10 cm-3 above 10 keV). These estimates pose serious questions for the thick-target interpretation. We will discuss alternative scenarios, including the idea of a purely non-thermal electron distribution as the source of the hard X-ray emission.

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