The Interstellar Medium and Formation of Stars

Skills
Present insight into the physics behind the temperature and density distributions of the different phases of the interstellar medium. Account for the key physical phenomenon such as shocks and PDRs as well as describe the underlying physical mechanisms dictating the structure and evolution of dense clouds. Demonstrate knowledge about the physics behind of the collapse of dense cores – including the importance and effects of thermal support, rotation, magnetic fields and turbulence. Describe the overall evolution of young stars including time-scales and key events such as the launching of jets and outflows and formation and evolution of protoplanetary disks. Account for the overall hypotheses regarding the processes leading to the formation of planets. For all of the above: show insight into the constraints obtainable from detailed observations as well as large numerical simulations.

Knowledge
The course follows the progression of the interstellar medium from the largest scales to planet forming regions. The first part of the course deals with the physics of the diffuse interstellar medium, and why it is so complex. An important issue is to understand the arguments for the existence of various phases with different densities. The second part is on aspects of the star formation itself and why the formation of Solar-type stars is interesting. The physical concepts will be demonstrated by selected exercises on star formation in nearby star forming molecular clouds: how is the collapse, taking place, how are protostars identified, how may their properties be derived?

Competences
This course will provide the students with a competent background for further studies within this research field, e.g. an M.Sc. project