From detailed magneto- convection simulations to modelling the convection zone-corona system Mats Carlsson Institute of Theoretical Astrophysics, University of Oslo Monterey February
Detailed simulations of magnetoconvection Optimization of observables Calibration of observables Interpretation Current status Future prospects Simulations of convection zone - corona
Nordlund/Stein code multi-group opacities, 4 bins Initial field 250G, vertical, single polarity 253x253x163 simulation RT each snapshot, 2728 frequency points Line blanketing: 845 lines MHD simulation of Solar magneto-convection
G-band spectral region Solar atlas Simulation
G-band synthetic image
Comparison with observations Simulation, mu=0.6 Observation, mu=0.63
Vertical velocity
Line wing Line center Velocity response function
Spectrum from simulation
Smeared with telescope+atm PSF
Observations
Velocity determination
Modelling coronal heating Magnetic field from MDI Potential field extrapolation Footpoint motion statistically described Conduction and thin losses included Chromosphere with artificial heating/cooling function Gudiksen & Nordlund 2005
Piecing it all together 16x8x12 Mm (2 Mm below, 10 Mm above) Open boundaries Multi-group opacities (4 bins) with scattering Conduction along field-lines Optically thin losses in corona Various initial magnetic field configurations Hansteen 2004
3D model from convection zone to corona
2D version nx=128, dx=130 km
2D version nx=512, dx= 32 km
Future modelling Convection zone multi-group opacities selected opacity sampling Magnetoconvection 20 km resolution, 6 Mm x 6 Mm 300x300 Supergranulation 48 Mm x 48 Mm, 50 km resolution 1000x1000
Future modelling Chromosphere Scattering approximate cooling in H, CaII, MgII time dependent H-ionization (implicit) CO chemistry (implicit) Corona Conduction along field lines (implicit)
Future modelling 3D Radiation MHD simulations from convection zone to corona necessary but also within reach Methodology known Several groups active Future of chromospheric modelling is promising!