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LMU/USM - Computational Star and Planet Formation Groups

We explore topics from the formation of planets and single stars to larger scale star and cluster formation by means of numerical and theoretical investigations. We use state-of-the-art numerical tools and develop new algorithms in-house in order to tackle problems of hydrodynamics, planet & disk interaction, planetesimal formation, dust & gas disk evolution, radiation transport in complex evolving hydrodynamical systems, and others. 

Some of the latest highlights from the groups involve

  • simulations of photoionisation feedback from young massive stellar clusters on the surrounding natal cloud
  • kinematic detection of young planets in comparison with simulations of planet-disk interaction
  • the dispersal of protoplanetary discs by energetic radiation from the central star and by planet formation
  • the escape of ioninsing radiation from galaxies in the context of IGM ionisation re-ionisation in the early universe
  • explaining high resolution dust continuum observations with models of dust evolution and planetesimal formation

PhD projects can be offered in the context of these research topics listed above. For more details visit the homepages of

Prof. Dr. B. Ercolano and

Prof. Dr. T. Birnstiel

Left: Bubbles and pillars sculpted by HII regions in a turbulent molecular cloud. Snapshot of the neutral gas from a Smooth Particle Hydrodynamic simulation performed by Jim Dale. Right: A Jupiter mass planet interacting with the gas (gray scale) and dust of the accretion disk. Large particles (blue, >1mm) collect in a pressure maximum outside the planet orbit and also at the center of a vortex. Small dust grains (red, <10 micrometer) exist everywhere, but in this case are locally enhanced in the vortex center by collisional fragmentation of large particles.