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 used to be Multi-Wavelength Observations of Coronal constitution and Dynamics. In those court cases the various and sundry advances of the dynamics sun surroundings long ago ten years of observations through Yohkoh were reviewed.
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Additional info for Multi-Wavelength Observations of Coronal Structure and Dynamics
The positive-polarity patches labeled D and F approach negative-polarity patches labeled A, B, and I after 19 November, and it appears that they are partially canceled. Associated with the cancellation, a new loop system connecting the positive-polarity area (D and F) to the negative-polarity area (A and B) is observed after 20 November. A magnetic bipole labeled B and C shows shearing motion; the negative patch B slowly separates from the positive patch C, and the direction of the line across B and C slightly rotates counterclockwise.
Also V~ _ 30 km s - l a t 1 AU in Figure 1 is close to observations. 1Hz or less. 1 T faculae (103 Gauss) is the source of the mechanical energy flux. In cylindrical coordinates we assume B = (0, B~, Bz) and V = (0, V~, 0). The twisting motion V~ 'in the corona' is nearly perpendicular to the main magnetic field Bz. Hence V~ produces almost-radial electric fields Er -- - ( Y x B ) r . This inevitably produces a non-zero divergence by 'definition' and a charge separation: a/r (7) = d i v E ~ OrEr/rOr = - B z O r V ~ / r O r .
The charges generate strong electric fields along the magnetic field, creating supra-thermal electron beams. Classical Coulomb collisions of these beams with ambient particles will heat the corona and start to accelerate the solar wind in accord with various observations. This is not Joule heating of any kind, but a co-spatial frictional heating. Thin sheaths and reconnections are not involved. ACCELERATION BY THE HEAT DEPOSITED AND THE MAGNETIC PRESSURE GRADIENT Simple Derivation of Terminal Velocity Here we try to understand, from empirical study, the basic physics of how the solar wind is accelerated.
Multi-Wavelength Observations of Coronal Structure and Dynamics by P. Martens, D. Cauffman