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
	The Team
	Solar Corona in 3D Group Homepage
	Solar Corona in 3D Publications by MPS Members

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	Thomas Wiegelmann (Group Speaker) Bernd Inhester
Post docs	Julia Thalmann Tilaye Tadesse
PhD Students	Judith de Patoul Iulia Chifu
IT specialist	Borut Podlipnik
Guest scientists	Narges Fathalian T. Neukirch D. Nickeler Nandita Srivastava
Former group members	Maxim Kramar Peng Ruan Li Feng