Wiegelmann, T.; Neukirch, T.: An optimization principle for the computation of MHD equilibria in the solar corona. Astronomy and Astrophysics 457, pp. 1053 - 1058 (2006)
Wiegelmann, T.; Xia, L. D.; Marsch, E.: Links between magnetic fields and plasma flows in a coronal hole. Astronomy and Astrophysics 432, pp. L1 - L4 (2005)
Marsch, E.; Wiegelmann, T.; Xia, L. D.: Coronal plasma flows and magnetic fields in solar active regions Combined observations from SOHO and NSO/Kitt Peak. Astronomy and Astrophysics 428, pp. 629 - 645 (2004)
Wiegelmann, T.; Solanki, S. K.: Similarities and differences between coronal holes and the quiet sun: are loop statistics the key? Solar Physics 225, pp. 227 - 247 (2004)
Carcedo, L.; Brown, D. S.; Hood, A. W.; Neukirch, T.; Wiegelmann, T.: A quantitative method to optimise magnetic field line fitting of observed coronal loops. Solar Physics 218, pp. 29 - 40 (2003)
Wiegelmann, T.; Inhester, B.: Magnetic modelling and tomography: First steps towards a consistent reconstruction of the solar corona. Solar Physics 214, pp. 287 - 312 (2003)
Wiegelmann, T.; Büchner, J.: Evolution of magnetic helicity under kinetic magnetic reconnection 2. B ≠ 0 reconnection. Nonlinear Processes in Geophysics 9 (2), pp. 139 - 147 (2002)
Wiegelmann, T.; Neukirch, T.: Including stereoscopic information in the reconstruction of coronal magnetic fields. Solar Physics 208, pp. 233 - 251 (2002)
Wiegelmann, T.; Büchner, J.: Evolution of magnetic helicity in the course of kinetic magnetic reconnection 1. B=0 reconnection. Nonlinear Processes in Geophysics 8 (3), pp. 127 - 140 (2001)
Wiegelmann, T.; Büchner, J.: Kinetic simultations of the coupling between current instabilities and reconnection in thin current sheets. Nonlinear Processes in Geophysics 7, pp. 141 - 150 (2000)
Wiegelmann, T.; Schindler, K.; Neukirch, T.: Helmet Streamers with Triple Structures: Simulations of resistive dynamics. Solar Physics 191 (2), pp. 391 - 407 (2000)
Wiegelmann, T.; Neukirch, T.; Büchner, J.: Particle code simulation - Tests and limits of Vlasov code simulations and its application to null-helicity and co-helicity reconnection. In: Space Plasma Simulation, pp. 58 - 61 (Eds. Büchner, J.; Dum, C.; Scholer, M.). Copernicus Gesellschaft 2001 (2001)
Koumtzis, A.; Wiegelmann, T.; Madjarska, M. S.: Computing the global coronal magnetic field during activity maximum and minimum with a newly developed nonlinear force-free Yin-Yang code. In: EGU General Assembly Conference Abstracts, pp. EGU - 17168. EGU General Assembly Conference Abstracts, Vienna, Austria, 2023. (2023)
Lagg, A.; Ishikawa, R.; Merenda, L.; Wiegelmann, T.; Tsuneta, S.; Solanki, S. K.: Internetwork Horizontal Magnetic Fields in the Quiet Sun Chromoshpere: Results from a Joint Hinode/VTT Study. In: The Second Hinode Science Meeting: Beyond Discovery - Torward Understanding, 327 (Eds. B., L.; M., C.; T., M.; J., M.; K., R.). (2009)
Raouafi, N.-E.; Solanki, S. K.; Wiegelmann, T.: Hanle Effect Diagnostics of the Coronal Magnetic Field: A Test Using Realistic Magnetic Field Configurations. In: Solar Polarization 5: In Honor of Jan Stenflo, pp. 429 - 434 (Eds. Berdyugina, S. V.; Nagendra, K. N.; Ramelli, R.). (2009)
How does our star heat its outer atmosphere, the solar corona, to unimaginable temperatures of up to 10 million degrees Celsius? With unprecedented observational data from ESA's Solar Orbiter spacecraft and powerful computer simulations, ERC starting grant awardee Pradeep Chitta intends to bring new momentum to the search for the coronal heating mechanism.
The research group “Solar Lower Atmosphere and Magnetism” (SLAM) studies the conditions and dynamic processes in the atmospheric layer between the solar surface (photosphere) and the overlying chromosphere, an approximately 2000 km thick gas layer.
The main research fields of the department "Sun and Heliosphere" are covered by the research groups "Solar and Stellar Coronae", "Solar Lower Atmosphere and Magnetism", "Solar and Stellar Magnetohydrodynamics" and "Solar Variability and Climate".