A view of the solar granulation at 200 nm
Results of a 3D radiation hydrodynamics simulation of solar surface convection
M.Steffen, Astrophysikalisches Institut Potsdam & S. Wedemeyer, Institut für Theoretische Physik und Astrophysik, Universität Kiel

gt57g44n53bm_2000_00b gt57g44n53bm_2000_0_63b gt57g44n53bm_2000_0_82b gt57g44n53bm_2000_0_93b
Quiet solar granulation at 200.0 nm, assuming pure continuum opacities Quiet solar granulation at 200.0 nm, assuming a line haze due to FeI (0 ev) depressing the true continuum by 63% Quiet solar granulation at 200.0 nm, assuming a line haze due to FeI (0 ev) depressing the true continuum by 81% Quiet solar granulation at 200.0 nm, assuming a line haze due to FeI (0 ev) depressing the true continuum by 91%
gt57g44n53bm_4445_00r gt57g44n53bm_2000_5_50b gt57g44n53bm_2000_5_70b gt57g44n53bm_2000_5_84b
Quiet solar granulation at 444.5 nm, assuming pure continuum opacities Quiet solar granulation at 200.0 nm, assuming a line haze due to FeI (5 ev) depressing the true continuum by 50% Quiet solar granulation at 200.0 nm, assuming a line haze due to FeI (5 ev) depressing the true continuum by 69% Quiet solar granulation at 200.0 nm, assuming a line haze due to FeI (5 ev) depressing the true continuum by 82%
Alternative color table Model gt57g44n53bm: non-grey radiative transfer, no chromosphere Back to main page