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Solar Corona in 3D
Plasma physics of the solar corona and solar wind
The magnetic field couples the solar interior with the photosphere and corona where it drives heating processes and eruptive phenomena like flares and coronal mass ejections. We developed sophisticated computer-codes to model the coronal magnetic field and plasma by nonlinear and self-consistent extrapolation techniques, stereoscopy and tomography.
Science Objectives
- Nonlinear force-free coronal magnetic field extrapolations
- Magnetic connectivity between photosphere, chromosphere and corona
- Coronal heating
- Monitoring of free magnetic energy to predict flares and CMEs
- Stereoscopy of active region loops, polar plumes and CMEs
- Coronal tomography and vector tomography
- Feature recognition techniques
- Selfconsistent stationary MHD-equilibria
- Current sheet formation and magnetic reconnection
The Team
Senior Scientists
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Thomas Wiegelmann (Group Speaker)
Bernd Inhester
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Post docs
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Julia Thalmann
Tilaye Tadesse
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PhD Students
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Judith de Patoul
Iulia Chifu
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IT specialist
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Borut Podlipnik
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Guest scientists
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Narges Fathalian
T. Neukirch
D. Nickeler
Nandita Srivastava
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Former group members
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Maxim Kramar
Peng Ruan
Li Feng
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