AG meeting 2017
Splinter Meeting Activity
Solar and stellar activity and variability
Time: Thursday September 21, 14:00-16:30 and 17:00-19:00
Convenors: H. Peter , M. Käpylä , P. Käpylä , N. Krivova , A. Reiners , S. Shapiro , J. Warnecke 
The activity of stars, including the Sun, is driven by the magnetic field generated in the dynamo process. When emerging at the surface the concentrations of the magnetic field change the brightness of the star. Expanding further into the upper atmosphere, they largely control its dynamics and heating. Understanding solar and stellar activity therefore requires modelling and observational studies from the stellar interior all the way to the chromosphere and corona. Significant progress over the last decade greatly improved our understanding of solar and stellar activity and variability. This is based on the availability of data from solar and stellar observations as well as in numerical modelling of the dynamo and of stellar atmospheres. In this splinter we plan to bring together observational and modelling studies of the magnetic activity and brightness variations from both, the solar and the stellar perspective.