Impulsive phenomena in a small active region

Details Impulsive phenomena in a small active region Impulsive phenomena in a small active region

Feb 1985

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985soph...95..297w&link_type=abstract

Solar Physics (ISSN 0038-0938), vol. 95, Feb. 1985, p. 297-310.

Physics

21

Extreme Ultraviolet Radiation, Solar Activity, Solar Corona, Spatial Distribution, Temporal Distribution, Chromosphere, Heating, Spectrograms

Scientific paper

The temporal and spatial variations of EUV emission from a small growing active region were investigated. Frequent localized short-term (about a few minutes) fluctuations in EUV emission were observed throughout the 7.2 hr interval when the most continuous observations were acquired. Approximately 20 percent of the 5-arcsec x 5-arcsec pixels had intensity variations exceeding a factor of 1.3 for the chromospheric L-alpha line, a factor of 1.5 for lines formed in the chromospheric-coronal transition region and a factor of 1.4 for the coronal Mg X line. A subflare in the region produced the largest intensity enhancements, ranging from a factor of about 2.3 for the chromospheric L-alpha line to about 8 for the transition region and coronal lines. The EUV fluctuations in this small active region are similar to those observed in coronal bright points, suggesting that impulsive heating is an important, perhaps dominant form of heating the upper chromospheric and lower coronal plasmas in small magnetic bipolar regions. The responsible mechanism most likely involves the rapid release of magnetic energy, possibly associated with the emergence of magnetic flux from lower levels into the chromosphere and corona.

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