Modeling Physical Processes in the ISM
--------------------------------------

1.    Introduction [~1h]

      - phenomenology of stellar birth 
      - short historic overview
      - complexity of star formation, overview of relevant physical processes

2.    ISM dynamics and of star formation [~4h]

      2.1 Turbulence
      
    	  - turbulence in the interstellar medium (statistical characteristics)
    	  - discussion of possible drivers of ISM turbulence
    	  - excursion: modeling turbulence
	  
      2.2 Gravo-turbulent star formation models

          - short overview of statistical (turbulence-based) star formation models
          - competitive accretion vs. monolithic collapse vs. alternative approaches

      2.3 Influence of density profile on star-cluster formation

          - dependence of fragmentation on initial density profile of cluster
          - forming cloud cores
          - requirement for taking cloud formation into account
     
      2.4 Radiative processes
      
          - coupling between gas/dust and the radiation field
          - long excursion: modeling radiative transfer
	  
      2.5 Thermodynamic properties of the ISM
      
          - main heating and cooling mechanisms
          - chemical processes in the ISM
          - multi-phase ISM
          - excursion: modeling extinction in dense clouds 
	  
      2.6 Magnetic fields in the ISM
      
          - influence of magnetic fields on molecular cloud dynamics 
          - protostellar collapse and magnetic fields

3. Star formation and feedback [~1.5h]

      - importance of feedback for locally terminating star formation
      - excursion: sink particles as subgrid-scale model of protostellar collapse
   
      3.1 Radiative feedback						      

          - accretion heating						    
          - ionizing radiation, HII regions				    
          - excursion: coupling (proto)stellar evolution to sink particles  
            								      
      3.2 Mechanical feedback						      

          - controversial role of outflows in star formation		    
          - excursion: modeling outflows				    

4. Some selected applications [~1.5h]

      4.1 The stellar initial mass function 
      
     	  - theoretical models of the IMF
     	  - universality
      
      4.2 Star formation in the primordial universe
      
     	  - formation of the first stars
     	  - transition from Population III to Population II (dust vs. atomic cooling lines)
     	  - observational constraints
	  
      4.3 Magnetic field amplification in the early universe
      
     	  - dynamo processes in primordial halos
     	  - some notes on numerical resolution