Spectral and spatial properties of solar microflares

Details Spectral and spatial properties of solar microflares Spectral and spatial properties of solar microflares

Aug 1985

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985icrc....4...38s&link_type=abstract

In its 19th Intern. Cosmic Ray Conf., Vol. 4 p 38-41 (SEE N85-34729 23-92)

Physics

Solar Corona, Solar Flares, Solar Protons, Solar X-Rays, Spectra, Electrons, Particle Acceleration, Plasmas (Physics)

Scientific paper

Solar microflares are studied using both hard ( 28 keV) and soft (3.5 to 8.0 keV) X-ray observations. The soft X-ray events have durations 3 m at 0.1x maximum intensity, and typically have similar rise and decay times. The fastest decay observed was 15 s (1/e). Soft and hard X-ray intensities are uncorrelated. The events are very compact, consistent with a projected area approximately 8 x 8 inches. They are normally not associated with H alpha or type 3 emissions and their time profiles suggest a thermal origin at the top of the chromosphere. If the primary energy release site is in the corona, an energy transfer agent consistent with the observations is a non-thermal proton beam.

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