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The robustness of cosmic-ray-induced H2 line emission on astrochemical model assumptions

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  • Figure 1: Line-of-sight line intensities of the 3d-pdr model (dense cloud) (top) and the SILCC-Zoom MHD cloud (bottom) for the four different H2 lines.
  • Figure 2: Logarithmic column-density bin-averaged line intensities versus the total H2 column density for the H2 lines. The blue and red lines correspond to 3d-pdr and SILCC-Zoom models, blue and red, respectively with the filled regions representing ±2σ. The black dashed-dot line shows the Neff-n 1D model. Black triangles show the observational upper limits on the (1-0)S(0) line from Bialy et al. (2022). The shadowed region shows the JWST sensitivity with a signal-to-noise ratio of 3 with 1.25 h of integration and 50 shutters (Padovani et al. 2022).

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