1. From detailed magneto- convection simulations to modelling the convection zone-corona system Mats Carlsson Institute of Theoretical Astrophysics, University of Oslo Monterey February 14 2006

2. Detailed simulations of magnetoconvection Optimization of observables Calibration of observables Interpretation Current status Future prospects Simulations of convection zone - corona

3. 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

4. G-band spectral region Solar atlas Simulation

5. G-band synthetic image

6. Comparison with observations Simulation, mu=0.6 Observation, mu=0.63

7. Vertical velocity

8. Line wing Line center Velocity response function

9. Spectrum from simulation

10. Smeared with telescope+atm PSF

11. Observations

12. Velocity determination

13. 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

14. 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

15. 3D model from convection zone to corona

16. 2D version nx=128, dx=130 km

17. 2D version nx=512, dx= 32 km

18. 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

19. Future modelling Chromosphere Scattering approximate cooling in H, CaII, MgII time dependent H-ionization (implicit) CO chemistry (implicit) Corona Conduction along field lines (implicit)

20. 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!