zum Inhalt springen

Cosmic Ray Attenuation and the Molecular Carbon Cycle

1 / 2
  • Fig. 1: Column densities of C+ (top), C (middle) and CO (bottom) for the attenuated CR model. Second to Fourth columns: The relative difference in column density for a constant CRIR with respect to the attenuated CR model for each of the aforementioned species.
  • Fig. 2: Velocity integrated emission of the [CII] 158 micron (top), [CI] 609 micron (middle) and CO (1-0) (bottom) emission in units of (K km/s). Second to Fourth columns: Relative emission for the different constant cosmic-ray ionization rate models with respect to the attenuated CR model.

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