April 8, 2013 to May 3, 2013
Europe/Stockholm timezone

Photo: Atefeh Barekat


The goal of the programme is to advance our understanding of the physical processes generating differential rotation in various types of stars, and the role that this effect plays for stellar magnetic activity and dynamos. The Sun is the only star for which the internal rotation profile is observationally known thanks to helioseismology – for other stars, only the surface differential rotation can be inferred from photometric or spectroscopic observations. Much relies on numerical models, working either under the mean-field approximation, or alternatively directly modelling rotating turbulent convection. The former approach has developed to the stage at which rotation profiles of different types of stars can be routinely calculated, although the effect of magnetic fields is normally not taken into account. Models of the latter category can quite satisfactorily produce the solar internal rotation profile, but calculations are computationally tremendously expensive, making large parameter studies very difficult. Analysis of observations, on the other hand, seems to indicate somewhat stronger, and sometimes anti-solar, differential rotation, as opposed to the predictions from mean-field models. This leaves quite uncertain grounds for further development of stellar dynamo theory, one of the key ingredients for the operation of the dynamo being the stellar nonuniform rotation. The main goal of the program is to investigate the connection between the theories and observations and obtain better understanding of the generation and role of differential rotation for stellar magnetism, and to formulate new theoretical, modeling and data analysis methods.

[Timetable - with slides of contributions]

Focus event

We are planning a one-week conference in the beginning of the program, which will be tightly focused to the topics addressed in the scientific case, but be open to a much larger number of participants. - Schedule of the conference

The conference takes place in the lecture rooms B2 and B3 of the building Brinellvägen 23 on the campus of Kungliga Tekniska Högskolan (KTH).

Other program activities

The work schedule for the remaining three weeks of the program consists of topical discussion sessions, seminars, and team work on issues raised during the focus event. These activities take place at Nordita and on the Albanova campus (top-left part of this PDF; we will mostly use building 23, but also building 33 "FP").

April 8 - April 12 Conference Differential Rotation and Magnetism across the HR Diagram
April 15 - April 19 Program week Generation and observation of differential rotation
April 22 - April 26 Program week Differential rotation interacting with magnetic fields (instabilities, torsional oscillations)
April 29 - May 03 Program week Dynamo processes in differentially rotating stars

Other activities

During the program, currently on three of the Fridays at 15:15-16:30, there astrobiology lectures, which may be of interest to some of the participants. There may also be some AlbaNova/Nordita colloquia on Thursdays, 15:15.

There is no registration fee.


Nordita provides a limited number of rooms in the Stockholm apartment hotel BizApartments free of charge for program participants.

Sponsored by:

Nordita Swedish Research Council