Radio and Hard X-Ray Images of High-Energy Electrons in an X-Class Solar Flare

Details Radio and Hard X-Ray Images of High-Energy Electrons in an X-Class Solar Flare Radio and Hard X-Ray Images of High-Energy Electrons in an X-Class Solar Flare

Oct 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003apj...595l.111w&link_type=abstract

The Astrophysical Journal, Volume 595, Issue 2, pp. L111-L114.

Astronomy and Astrophysics

Astronomy

27

Sun: Corona, Sun: Flares, Sun: Radio Radiation

Scientific paper

We present the first comparison between radio images of high-energy electrons accelerated by a solar flare and images of hard X-rays produced by the same electrons at photon energies above 100 keV. The images indicate that the high-energy X-rays originate at the footpoints of the loops dominating the radio emission. The radio and hard X-ray light curves match each other well and are quantitatively consistent with an origin in a single population of nonthermal electrons with a power-law index of around 4.5-5. The high-frequency radio spectral index suggests a flatter energy spectrum, but this is ruled out by the X-ray spectrum up to 8 MeV. The preflare radio images show a large hot long-lived loop not visible at other wavelengths. Flare radio brightness temperatures exceed 109 K, and the peak in the radio spectrum is as high as 35 GHz: both these two features and the hard X-ray data require very high densities of nonthermal electrons, possibly as high as 1010 cm-3 above 20 keV at the peak of the flare.

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