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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] ph1.uni-koeln.de

Consultation hours

upon agreement in Room 1.14, Building 312 

The origin of Non-thermal Radio Filaments observed in the Galactic Centre

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  • Figure 1: The slice of the density, pressure, and magnetic field distribution (from top to bottom) along the z-axis of the comet-like filament in the ISM (left), harp-like filament in the ISM (middle), and the harp-like filament in the CMZ (right). The distributions are shown in the stellar rest frame. The arrows in the magnetic field distributions indicate the direction of the magnetic field.
  • Figure 2: The time-integrated synchrotron intensity for the three configurations considered in this project, shown in the laboratory frame. The intensity is normalised by the maximum intensity in each distribution. The comet-like and harp-like filaments (Adapted from Heywood et al. 2022, ApJ *925* 165 and Thomas et al. 2020 ApJ *890* 2) are also overlayed on the left of the distribution.