Institute of Astronomy,

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Micro-events in the Solar Corona
(activequiet) Arnold O. Benz Paolo Grigis
Institute of Astronomy, Radio Astronomy and
Plasma Physics Group
Eidgenössische Technische Hochschule Zürich Swiss
Federal Institute of Technology, Zürich
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Spectral and spatial
properties of solar microflares
Simnett, G. M. Dennis, B. R.
In its 19th Intern. Cosmic Ray Conf.,
Vol. 4 p 38-41 (SEE N85-34729 23-92)
08/1985 Solar
Physics 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.
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Spectral and spatial
properties of solar microflares
Simnett, G. M. Dennis, B. R.
In its 19th Intern. Cosmic Ray Conf.,
Vol. 4 p 38-41 (SEE N85-34729 23-92)
08/1985 Solar
Physics 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.
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active region
GOES 1.6-12.4 keV
A
B
RHESSI 3 -15 keV
2 May 2002
Benz Grigis, 2002
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active region
RHESSI, 2 May 2002
Benz Grigis, 2002
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active region
Event A
RHESSI, 2 May 2002
Benz Grigis, 2002
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stellar flare gt
dMe, dKe and RS CVn stars gt
gradual flares gt
impulsive flares gt
microflares, active region gt
nanoflares, quiet region gt
Benz Güdel, 1996 Krucker Benz, 2000
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3 9 keV, 60 minutes RHESSI
magnetogram MDI/SOHO
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