Slide 1 ISM Lecture 13 H 2 Regions II: Diffuse molecular clouds; C + => CO transition Slide 2 13.1 Diffuse molecular clouds Diffuse clouds clouds with total visual…
ISM Lecture 10 The Three-Phase Interstellar Medium 10.1 Why necessary? Two-phase model (see Sect. 8.3) FGH model: Heating by cosmic rays => p.e. effect UV from stars:…
ISM Lecture 9 Shock waves; Supernova remnant evolution 9.1 Shock waves A shock wave is a pressure-driven compressive disturbance propagating faster than “signal speed”…