Dynamo theory explains why the plasma in our universe is magnetized. As we now know, astrophysical turbulence without magnetic fields does not exist. This has dramatic consequences, especially when the magnetic Prandtl number (PrM) is very different from unity. Examples include the interstellar medium and especially clusters of galaxies, where PrM is huge, and much of the energy dissipation goes into particle acceleration. In galaxy clusters, we also reach the limits of validity of magnetohydrodynamics (MHD) and thus need to worry about the correct microphysical description. In the Sun, a large-scale dynamo is most likely operational within the bulk of the convection zone,where the thermal and magnetic Prandtl numbers are small, but this situation drastically changes as the surface and atmosphere are reached. Here, PrM is large and a dynamo operates arguably in reverse, because now energy flows from magnetic into kinetic energy, and this contributes to heating the corona, for example. Again, kinetic effects can become important. Simulating these aspects correctly on the computer requires special care, which we are only now beginning to appreciate. The goal is to use Nordita’s inhouse expertise in the field of dynamo theory to draw together experts from within the Nordic countries and elsewhere to prepare the way for new work.
(password to be communicated via email)
The colloquia on Thursdays at 15:15 (https://indico.fysik.su.se/category/301/) are in the Oskar Klein Auditorium in the AlbaNova main building and usually also on https://stockholmuniversity.zoom.us/j/62663587311
On May 19, the Oskar Klein Lecture will be delivered by Igor Klebanov in the Oskar Klein Auditorium in the AlbaNova main building and is also on https://stockholmuniversity.zoom.us/j/63385615405. Note that there is a reception with finger food afterwards.
Some of the Friday talks of the astronomy department at 10:30 may be of interest and are in the 6th floor of the astronomy department in FC61 and also on https://stockholmuniversity.zoom.us/j/68066058145
Themes and program schedule
Timetable of the programme can be found here.
We intend to organize the program around the following themes:
Week 1 - Kinetic effects in solar surface layers and reprocessing of dynamo-generated fields
Week 2 - Toward collisionless dynamos in galaxy clusters: numerical approaches and results
Week 3 - New large-scale dynamo effects, especially in shearing environments
Week 4 - Toward a multiscale approach in stellar dynamos, plus focus event
In this time of the year, there are several public holidays (Thursday May 26 and Monday June 6). The program will run as scheduled, but the usual lunch places won't be open and busses run on the Sunday schedule. If you don't get in, call Axel on +46 73 270 4376. He may arrange for an improvised pizza lunch on those days.
Registration to be considered for on-site participation will close on March 25th. Registrants will then receive an on-site/remote participation confirmation from the organizers. Any registration made after the 25th of March will be considered as a registration for remote participation.