from detailed magneto- convection simulations to modelling the convection zone-corona system mats...
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![Page 1: From detailed magneto- convection simulations to modelling the convection zone-corona system Mats Carlsson Institute of Theoretical Astrophysics, University](https://reader036.vdocuments.us/reader036/viewer/2022062804/56649d4d5503460f94a2c8d5/html5/thumbnails/1.jpg)
From detailed magneto-convection simulations to modelling the
convection zone-corona system
Mats CarlssonInstitute of Theoretical Astrophysics,
University of OsloMonterey February 14 2006
![Page 2: From detailed magneto- convection simulations to modelling the convection zone-corona system Mats Carlsson Institute of Theoretical Astrophysics, University](https://reader036.vdocuments.us/reader036/viewer/2022062804/56649d4d5503460f94a2c8d5/html5/thumbnails/2.jpg)
Detailed simulations of magnetoconvection
•Optimization of observables
•Calibration of observables
•Interpretation
•Current status
•Future prospects
Simulations of convection zone - corona
![Page 3: From detailed magneto- convection simulations to modelling the convection zone-corona system Mats Carlsson Institute of Theoretical Astrophysics, University](https://reader036.vdocuments.us/reader036/viewer/2022062804/56649d4d5503460f94a2c8d5/html5/thumbnails/3.jpg)
•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
![Page 4: From detailed magneto- convection simulations to modelling the convection zone-corona system Mats Carlsson Institute of Theoretical Astrophysics, University](https://reader036.vdocuments.us/reader036/viewer/2022062804/56649d4d5503460f94a2c8d5/html5/thumbnails/4.jpg)
G-band spectral region
Solar atlasSimulation
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G-band synthetic image
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Comparison with observations
Simulation, mu=0.6Observation, mu=0.63
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Vertical velocity
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Line wingLine center
Velocity response function
![Page 9: From detailed magneto- convection simulations to modelling the convection zone-corona system Mats Carlsson Institute of Theoretical Astrophysics, University](https://reader036.vdocuments.us/reader036/viewer/2022062804/56649d4d5503460f94a2c8d5/html5/thumbnails/9.jpg)
Spectrum from simulation
![Page 10: From detailed magneto- convection simulations to modelling the convection zone-corona system Mats Carlsson Institute of Theoretical Astrophysics, University](https://reader036.vdocuments.us/reader036/viewer/2022062804/56649d4d5503460f94a2c8d5/html5/thumbnails/10.jpg)
Smeared with telescope+atm PSF
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Observations
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Velocity determination
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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
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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
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3D model from convection zone to corona
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2D version
QuickTime™ and aGIF decompressor
are needed to see this picture.
nx=128, dx=130 km
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2D version
QuickTime™ and aGIF decompressor
are needed to see this picture.
nx=512, dx= 32 km
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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
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Future modelling•Chromosphere
•Scattering
•approximate cooling in H, CaII, MgII
•time dependent H-ionization (implicit)
•CO chemistry (implicit)
•Corona
•Conduction along field lines (implicit)
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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!