Feng, L.; Inhester, B.; Wang, Y.; Shen, F.; Shen, C.; Gan, W.: On the mass evolution of CMEs. European Solar Physics Meeting 14, Dublin, Ireland (2014)
Curdt, W.; Inhester, B.: Schlussbericht zum Vorhaben ``Operation des SUMER-Instrumentes und Routine-Auswertung LASCO im Rahmen der Solar Cycle Mission''. Max-Planck-Institut für Sonnensystemforschung, Katlenburg-Lindau, Germany (2009)
Michels, D. J.; Schwenn, R.; Howard, R. A.; Bartoe, J.-D. F.; Antiochos, S. K.; Brueckner, G. E.; Dere, K. P.; Doschek, G. A.; Mariska, J. T.; Sheeley Jr., N. R.et al.; Socker, D. G.; Daly, P. W.; Inhester, B.; Keller, H.-U.; Kramm, J. R.; Rosenbauer, H.; Lamy, P.; Llebaria, A.; Maucherat, A.; Parker, E. N.; Kahler, S. W.; Koutchmy, S. L.; Smartt, R. N.; Wagner, W. J.; Bougeret, J.-L.; Pick, M.; Noens, J.-C.; Giese, R. H.; Koomen, M. J.; Giovane, F.; Misconi, N. Y.: A wide-field white light and spectrometric coronagraph for SOHO. NRL Washington, MPAe Katlenburg-Lindau, LAS Marseille (1987)
Analyzing the high spatial resolution solar Ca II H and K emission data obtained by the SUNRISE mission and building a model of other stars more active than the Sun
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.