1. Micro-events in the Solar Corona (active+quiet)
Arnold O. Benz
Paolo Grigis
Institute of Astronomy,
Radio Astronomy and Plasma Physics Group
Eidgenössische Technische Hochschule Zürich
Swiss Federal Institute of Technology, Zürich

2. Spectral and spatial properties of solar microflares
Simnett, G. M.; Dennis, B. R.
In its 19th Intern. Cosmic Ray Conf., Vol. 4 p (SEE
N )
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.

3. Spectral and spatial properties of solar microflares
Simnett, G. M.; Dennis, B. R.
In its 19th Intern. Cosmic Ray Conf., Vol. 4 p (SEE
N )
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.

5. A B active region GOES 1.6-12.4 keV RHESSI 3 -15 keV 2 May 2002
Benz & Grigis, 2002

6. active region
RHESSI, 2 May 2002
Benz & Grigis, 2002

7. active region
Event A
RHESSI, 2 May 2002
Benz & Grigis, 2002

13. stellar flare =>
dMe, dKe and RS CVn stars =>
gradual flares =>
impulsive flares =>
microflares,
active region =>
nanoflares,
quiet region =>
Benz + Güdel, 1996
Krucker + Benz, 2000

14. 3 – 9 keV, 60 minutes
RHESSI
magnetogram
MDI/SOHO