Işık, E.; Holzwarth, V.: Flow instabilities of magnetic flux tubes IV. Flux storage in the solar overshoot region. Astronomy and Astrophysics 508 (2), pp. 979 - U479 (2009)
Holzwarth, V.; Schüssler, M.; Schmitt, D.: Flow instabilities of magnetic flux tubes - II. Longitudinal flow. Astronomy and Astrophysics 469, pp. 11 - 17 (2007)
Holzwarth, V.; Schüssler, M.: Dynamics of magnetic flux tubes in close binary stars I. Equilibrium and stability properties. Astronomy and Astrophysics 405, pp. 291 - 301 (2003)
Holzwarth, V.; Schüssler, M.: Dynamics of magnetic flux tubes in close binary stars II. Nonlinear evolution and surface distributions. Astronomy and Astrophysics 405, pp. 303 - 311 (2003)
Holzwarth, V.; Schüssler, M.: Buried magnetic flux tubes in giant stars near the ``Coronal Dividing Line''. Astronomy and Astrophysics 377, pp. 251 - 263 (2001)
Holzwarth, V.: Magnetic flux emergence in fast rotating stars. In: Coronae of stars and accretion disks, pp. 271 - 278 (Eds. Massi, M.; Preibisch, T.). Memorie della Società Astronomica Italiana (2007)
Holzwarth, V.; Jardine, M.: Mass loss rates and wind ram pressures of cool stars. In: Modern Solar Facilities - Advanced Solar Science, pp. 371 - 374 (Eds. Kneer, F.; Puschmann, K. G.; Wittmann, A. D.). Universitätsverlag Göttingen (2007)
Holzwarth, V.; Schüssler, M.: Preferred longitudes of starspots on magnetically active close binaries. In: Magnetic Fields Across the Hertzsprung-Russell Diagram, pp. 247 - 250 (Eds. Mathys, G.; Solanki, S. K.; Wickramasinghe, D. T.). Astronomical Society of the Pacific, San Francisco, USA (2001)
Holzwarth, V.; Schüssler, M.; Solanki, S. K.: A model for the decline of coronal X-ray emission of cool giant stars. In: Magnetic Fields Across the Hertzsprung-Russell Diagram, pp. 259 - 262 (Eds. Mathys, G.; Solanki, S. K.; Wickramasinghe, D. T.). Astronomical Society of the Pacific, San Francisco/CA (2001)
Schüssler, M.; Holzwarth, V.; Solanki, S. K.; Charbonnel, C.: Buried flux tubes in the coronal graveyard. In: Cool Stars, Stellar Systems and the Sun, pp. CD - 1114 (Eds. López, G.; J., R.; Rebolo; R.; Osorio, Z. et al.). Astronomical Society of the Pacific, San Francisco (2001)
The magnetic field in the solar atmosphere exceeds the geomagnetic field strength by four orders of magnitude. It greatly influences the processes of energy transport within the solar atmosphere, and dominates the morphology of the solar chromosphere and corona. Kinetic energy from convective motions in the Sun can be efficiently stored in magnetic fields and subsequently released - to heat the solar corona to several million degrees or to blast off coronal mass ejections.
The Solar Lower Atmosphere and Magnetism (SLAM) group covers many exciting subjects in solar physics, focussing on the development and testing of highly novel solar instrumentation, reduction and analysis of highest quality solar observations, or improving and developing advanced techniques for the analysis of solar observations.
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".
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.