The course covers the physical processes that dominate in the interstellar medium. In particular, it covers
photoionization, recombination, line emission, continuum emission, dust and shocks. Applications are made
for planetary nebulae, supernova remnants, interstellar clouds, stellar winds and active galaxies.It is expected that the student after taking the course will be able to: - know and understand the physical
processes that dominate in the interstellar medium and other similar gases - to estimate temperature and
ionization/excitation conditions in such gases and the temperature in dust that may exist - describe which
components that exist in the interstellar medium, their properties, and which of them that are in rough
pressure equilibrium and which of them are not - show understanding for the types of shocks that may exist in
the interstellar medium - show ability to independently acquire knowledge about the physical processes that
are treated in the course, as well as in an independent way communicate this knowledge to other students and
the teachers - interpret spectral information from the emission and absorption of radiation which is produced
in the interstellar medium and other similar gases.
