As shown by observations, many young stars (age<5-10 Myr) harbor a circumstellar disk and accrete material from it through the star-disk magnetosphere. Despite the large amount of observational data in the infrared, optical and X-ray bands, different issues regarding star-disk interactions are still yet open. Many of these issues need detailed physical models of the star-disk system for a better insight. To this end, we are developing a model describing the interaction between the accreting material and the star atmosphere, using the 3D Magneto-HydroDynamical (MHD) code PLUTO developed at the University of Torino. We plan to perform a set of demanding simulations on the PI2S2 Grid infrastructure. Here, we describe the model, the main features on the most recent PLUTO version which we ported on the Grid and the first runs of the PLUTO code performed on the PI2S2 Grid.
|Numero di pagine||4|
|Stato di pubblicazione||Published - 2008|