Imaging spectra of hard X-rays from the footpoints of solar impulsive loop flares

Details Imaging spectra of hard X-rays from the footpoints of solar impulsive loop flares Imaging spectra of hard X-rays from the footpoints of solar impulsive loop flares

Jun 1995

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995pasj...47..355t&link_type=abstract

PASJ: Publications of the Astronomical Society of Japan (ISSN 0004-6264), vol. 47, no. 3, p. 355-364

Astronomy and Astrophysics

Astronomy

12

Coronal Loops, Solar Flares, X Ray Astronomy, X Ray Imagery, X Ray Spectra, Brightness Distribution, Flux Density, Image Analysis, Japanese Spacecraft, Spectrum Analysis, X Ray Telescopes

Scientific paper

The imaging spectra of hard X-rays emitted from one or both footpoints of solar impulsive loop flares seem to frequently show a better fit to an extremely hot thermal spectrum, on the order of 108 K, than to a power-law spectrum, in the main phase of the bursts. In the present study of tendency has been verified by the spectra of nine impulsive bursts having a sufficient flux for reliable imaging in the H-band (52.7-92.8 keV) of the hard X-ray telescope (HXT) aboard the Yohkoh spacraft. The spectral indexes at the footpoints were derived from the hard X-ray images in four energy bands of the HXT; their reliability was verified by mapping simulations. Since the X-ray spectrum depends on the location in the X-ray loop, the spectrum of the total flux is generally different from the spatially resolved spectra. The imaging spectrum is thus crucial for studying the nature of the electrons emitting hard X-rays. The heat conduction of an extremely hot quasi-thermal plasma seems to play an essential role in impulsive loop flares.

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