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Effect of stellar feedback on star formation in Dwarf Galaxies

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  • Enlarged view:
    Video: Time evolution of the column density of two simulations including supernova feedback from massive stars where the simulation in the left panel also includes radiation feedback. The dots represent sinks which contain massive stars where the color represents the total number of massive stars in the sink (black ∼1, redder > 1). The top and bottom panel represent the edge and face on view respectively.
  • Enlarged view:
    Time evolution of the mean number of massive stars per sink for simulations with different feedback mechanisms (R-radiation, W-wind, SN-supernova) and different sink creation criteria. The brown and purple line represent the two simulations from the video.

Theoretical Astrophysics group Cologne - TAC

Our research deals with the numerical modelling of the star formation process by means of high-performance, 3D, magneto-hydrodynamical (MHD) simulations. The simulations cover large spatial scales from ISM physics on kpc scales over molecular clouds on scales of 10 - 100 pc to star forming filaments on (sub-) pc scales and finally to protostellar discs and jets on scales of 10 - 1000 AU.

In our research group we use several tools like the (M)HD codes FLASH, GADGET, GANDALF , the astrochemical code KROME, 3D-PDR or radiative transport codes like RADMC-3D and POLARIS.

Prof. Dr. Stefanie Walch-Gassner is the head of the SILCC project (SImulating the life Cyle of molecular Clouds), a collaboration of several European astrophysical institutes, which has set the aim to model the formation, evolution, and dispersal of molecular clouds in 3D, MHD simulations with particular focus on a detailed astro-chemical modelling and the inclusion of various feedback processes.

Contact information:

  • Phone: (+49|0) 221 / 470 - 3497
  • Fax: (+49|0) 221 / 470 - 5162
  • Email: walch [at]

Consultation hours

upon agreement in Room 1.14, Building 312