zum Inhalt springen

Aluminum-26 Production in Protostellar Disks

1 / 2
  • Figure 1: This figure shows a schematic of the proposed mechanism. We denote a gas parcel on the surface of the disk, which is free-falling across the disk, as the red 'cluster'. The gas is then accreted onto the protostar, then recycled through the outflow and splash back. The regions indicated show different regimes of energetic particle transport.
  • Figure 2: 26Al/27Al as a function of protostellar mass for different constant accretion rates for our Fiducial model. The dotted lines show the canonical 26Al/27Al ratio measured in CAIs. The hatched region shows the range of values on Solar system chondrites.

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