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Bridge, H. S.; Belcher, J. W.; Lazarus, A. J.; Sullivan, J. D.; Bagenal, F.; McNutt Jr., R. L.; Ogilvie, K. W.; Scudder, J. D.; Sittler, E. C.; Vasyliūnas, V. M.et al.; Goertz, C. K.: Plasma observations near Jupiter: Initial results from Voyager 2. Science 206, pp. 972 - 976 (1979)
Bridge, H. S.; Belcher, J. W.; Lazarus, A. J.; Sullivan, J. D.; McNutt, R. L.; Bagenal, F.; Scudder, J. D.; Sittler, E. C.; Siscoe, G. L.; Vasyliūnas, V. M.et al.; Goertz, C. K.; Yeates, C. M.: Plasma observations near Jupiter: Initial results from Voyager 1. Science 204, pp. 987 - 991 (1979)
Dessler, A. J.; Vasyliūnas, V. M.: The magnetic anomaly model of the Jovian magnetosphere: Predictions for Voyager. Geophysical Research Letters 6, pp. 37 - 40 (1979)
Gonzalez, W. D.; Parker, E. N.; Mozer, F. S.; Vasyliūnas, V. M.; Pritchett, P. L.; Karimabadi, H.; Cassak, P. A.; Scudder, J. D.; Yamada, M.; Kulsrud, R. M.et al.; Koga, D.: Fundamental Concepts Associated with Magnetic Reconnection. In: Magnetic Reconnection, Vol. 427, pp. 1 - 32 (Eds. W., G.; E., P.). Springer, Switzerland (2016)
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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
For PhD students whose project is already funded and who are applying for admission to the IMPRS, or for applicants who want to bring their own funding and their own project idea to the IMPRS.
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.