Supported by the European Commission, Sixth Framework Programme - Marie Curie Conferences and Training Courses - MSCF-CT-2003-503674
Magnetic activity in a star like the Sun gives rise to dark spots, bright flares, mass ejections, dramatically enhanced radiation (from the radio to the EUV and X-ray), and copious production of highly accelerated particles, all of which are caused by fields generated in the star's interior. The course will cover the interaction between convection, rotation and magnetic fields in solar-type stars with deep outer convection zones. The aim will be to confront theory with observations. This is timely because new observations (from space and from the ground) are revealing fine details of surface features, while helio- and astero- seismology provide a means of probing stars' internal structure. Meanwhile, theoretical models are becoming more realistic and sophisticated, and the availability of ever more powerful computers has at last made it feasible to model nonlinear processes in sufficient detail. These results are explained by reference to precise mathematical models, describing the essential processes that are involved, and there is a strong overlap with nonlinear dynamics, including bifurcation theory and pattern formation.
The programme will contain lectures by leading figures that will cover a full range of theoretical topics, including solar magnetic fields, stellar activity, helioseismology and asteroseismology, protostellar activity, brown dwarfs, magnetoconvection, magnetoturbulence, shear and differential rotation, dynamos, stellar magnetic activity, cycles and grand minima, together with a survey of relevant observations and experiments.
There will also be opportunities for further shorter presentations.