HR: 1330h
AN: SH22A-0190    [PDF]
TI: Shear-Flow Reconnection Causing EUV Bright Point Heating
AU: * Buechner, J
EM: buechner@linmpi.mpg.de
AF: Max-Planck-Institut, Max-Planck-Str. 2, Katlenburg-Lindau, 37191 Germany
AU: Nikutowski, B
EM: nikutow@linmpi.mpg.de
AF: Max-Planck-Institut, Max-Planck-Str. 2, Katlenburg-Lindau, 37191 Germany
AU: Otto, A
EM: ao@how.gi.alaska.edu
AF: Geophysical Institute, University of Fairbanks, Fairbanks, AK 99775 United States
AB: EUV/X-ray Bright Points indicate permanent heating processes in the solar atmosphere. We used the information of observed magnetic fields and photospheric motion to simulate numerically by a global MHD approach, coupled to an appropriate kinetic model desrcibing dissipation, the physical processes behind the heating of the solar atmosphere. It appears that shear flow reconnection near the transition region is the main candidate to understand the localized heating behind Bright Points.
DE: 3210 Modeling
DE: 7507 Chromosphere
DE: 7524 Magnetic fields
DE: 7835 Magnetic reconnection
DE: 7843 Numerical simulation studies
SC: SPA - Solar and Heliospheric Physics [SH]
MN: 2003 Fall Meeting