HR: 0830h
AN: SP41A-01    [Abstracts]
TI: Heating of the Quiet Solar Corona
AU: * Hansteen, V H
EM: viggoh@astro.uio.no
AF: Institute of Theoretical Astrophysics, PB 1029 Blindern, Oslo, NA N - 0315 Norway
AU: * Hansteen, V H
EM: viggoh@astro.uio.no
AF: Center of Mathematics for Applications, PB 1053 Blindern, Oslo, NA N - 0316 Norway
AU: Gudiksen, B W
EM: boris@astro.uio.no
AF: Institute of Theoretical Astrophysics, PB 1029 Blindern, Oslo, NA N - 0315 Norway
AU: Gudiksen, B W
EM: boris@astro.uio.no
AF: Center of Mathematics for Applications, PB 1053 Blindern, Oslo, NA N - 0316 Norway
AB: A major goal in solar physics has during the last five decades been to find how energy flux generated in the solar convection zone is transported and dissipated in the outer solar layers. Progress in this field has been slow and painstaking. However, advances in computer hardware and numerical methods, vastly increased observational capababilities and growing physical insight seem finally to be leading towards understanding. We present numerical simulations of quiet sun heating that span the entire solar atmosphere from the upper convection zone to the lower corona. These models include non-grey, non-lte radiative transport in the photosphere and chromosphere, optically thin radiative losses as well as magnetic field-aligned heat conduction in the transition region and corona. The relation between the mean magnetic field strength and structure and the heating of the corona is discussed.
DE: 7507 Chromosphere
DE: 7509 Corona
DE: 7529 Photosphere
DE: 7546 Transition region
SC: Solar Physics Division - AAS [SP]
MN: 2005 Joint Assembly