By P. Martens, D. Cauffman
Those are the complaints of the Yohkoh tenth Anniversary assembly, a COSPAR Colloquium held in Kona, Hawaii, united states, on January 20-24, 2002. The identify of the assembly used to be Multi-Wavelength Observations of Coronal constitution and Dynamics. In those court cases the various and sundry advances of the dynamics sunlight surroundings long ago ten years of observations by way of Yohkoh were reviewed.
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Extra info for Multi-Wavelength Observations of Coronal Structure and Dynamics: Yohkoh 10th Anniversary Meeting: Proceedings of the COSPAR Colloquium Held in Kona, Hawaii, USA, 20-24 January 2002
Yokoyama & Shibata (1996) performed numerical simulations of such a reconnection jet. Polar UV jets could be produced as their anemone type of jet in the vertical coronal field. The simulations predict formation of a cool jet together with a hot one. EIT 195 /~ observations from 1996 July 13 revealed a macrospicular dark surge that occurred at the end of the UV jet sequence, at the base of the jet. ACKNOWLEDGEMENTS This work is supported by NASA under grant NAG5-10093 to the Smithsonian Astrophysical Observatory, by Agenzia Spaziale Italiana, and by the ESA PRODEX program (Swiss contribution).
Plunkett, and D. J. Michels, Evolution of global-scale coronal magnetic field due to magnetic reconnection, Astrophys. , 545, 1101 (2000). Zirker, J. , Coronal Holes and High-speed Wind Streams, Colorado Assoc. Univ. Press, Boulder (1977). -12- SOLAR WIND ACCELERATION, CRITICAL POINTS AND MASS FLUX, AND CORONAL HEATING DUE TO SUPRA-THERMAL ELECTRON BEAMS T. Hirayama Meisei University, Ome-shi, Tokyo, 198-8655, Japan ABSTRACT We present a simple steady model of the solar wind, where its acceleration is governed by the gas pressure gradient resulting from heating at lower altitudes, and by the magnetic pressure gradient at larger distances.
Weak transient activities are more easily found in quiet regions because of the low quasi-steady X-ray background level. No significant differences except for the involved energy and occurrence location may be found among X-ray transient brightenings, XBP flares (Strong et al. 1992, Kundu et al. 1994), network flares (Krucker et al. 1997), and EUV transient brightenings (Berghmans et al. 1998, Krucker & Benz 1998, Benz & Krucker 1998). The durations of these activities are all less than roughly 10 min, and they show soft X-ray light curves with a sudden increase at the beginning and a slow decrease in the late phase, which are temporal behaviors similar to those of standard flares.