Multi-Wavelength Observations of Coronal Structure and by P. Martens, D. Cauffman

Multi-Wavelength Observations of Coronal Structure and by P. Martens, D. Cauffman

By P. Martens, D. Cauffman

Those are the lawsuits of the Yohkoh tenth Anniversary assembly, a COSPAR Colloquium held in Kona, Hawaii, united states, on January 20-24, 2002. The name of the assembly was once Multi-Wavelength Observations of Coronal constitution and Dynamics. In those complaints the numerous and sundry advances of the dynamics sunlight surroundings some time past ten years of observations via Yohkoh were reviewed.

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These observarious have provided new views for understanding magnetic origins of the heating of transient and steady structures in the corona. It has been well known that the location and strength of identifiable X-ray features in the corona are associated with strong magnetic fields at the surface. Bright features seen in soft X-rays are located above sunspot groups observed in visible light. Yohkoh observations have quantitatively confirmed that the thermal properties of the "active-region" corona are well correlated to the integrated and averaged magnetic properties derived from magnetogram observations.

They are ejected with broad distributions of initial velocities - the leading edge moves with speeds of 400 - 1100 km s -1 and the "centroid" with average initial speed of 500 km s -1. As the jets travel they decelerate and are incorporated into the ambient solar wind within the C2 field of view (Wang et al. 1998). In this paper we present results of simultaneous SXT and UVCS observations of polar jets in December 1996. = 27 ~ UVCS/SOHO was obtaining synoptic observations at that time. 5 R e. = 45 ~ began at 12:06 UT.

1. This is because V stays finite as seen in Eq. 2. Since LD(r) is uncertain, Eq. 3 is, except for the lowest corona, accurate enough for 'the velocity', by far the most important parameter in the solar wind energetics. This implies that 'higher temperature' is not a necessary requirement of 'faster' flows. We regard the source velocity of the solar wind as an evaporating velocity due to excess heating of the transition region as in flares (see Paper I on closed loops). Cause of the Fast Wind Acceleration pvdV GM| dz + p ~ z The steady momentum equation is dP = - d--~ + (j x B)z.

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