Astronomy and Astrophysics – Astronomy
Scientific paper
Jun 1995
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995sowi.conf...28s&link_type=abstract
National Astronomical Observatory, International Solar Wind 8 Conference, p. 28
Astronomy and Astrophysics
Astronomy
Solar Corona, Solar X-Rays, Magnetic Field Reconnection, Solar Magnetic Field, Plasma Jets, Morphology, Coronal Loops, Solar Wind
Scientific paper
The Soft X-ray Telescope (SXT) aboard Yohkoh has revealed that the solar corona is much more dynamic that had been thought. Among various newly discovered dynamic phenomena, one of the most surprising findings is the discovery of coronal x-ray jets. The length of these jets is a few 103 - a few 105 km, their (apparent) velocity is a few 10 - a few 100 km/s (some reached 1000 km/s), and the corresponding kinetic energy is estimated to be 1025 - 1028 erg. They occur in association with small flares in active regions, emerging flux regions, and x-ray bright points, and show the following common characteristics: recurrency, whip-like motion, change in morphology at the footpoint ARs, and often converging (or inverted-Y) shape. Large scale loop brightenings observed by SXT seem to correspond to jets occurring in closed loop systems. These observations suggest that the magnetic reconnection between the emerging magnetic flux (or expanding loop) and the overlying coronal/chromospheric magnetic field is a key physical process for producing these jets. We shall summarize characteristics of these coronal X-ray jets observed by SXT, and also discuss the theoretical interpretation of them, especially in the framework of a magnetic reconnection model.
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