RESEARCH GROUP

2016

 

Dr. Daniel Seifried

Postdoctoral Researchers

PhD Students

Annika Franeck

Sebastian Haid

Dominik Derigs

Prabesh Raj Joshi

Nassim Tanha

Former Members

Dr. Jonathan Mackey

Dr. Andrea Gatto

Master Students

Paul Rohde

Thorsten Balduin

Peter Gerliz

Jonas Sonnabend (external, together with Prof. Dr. Schlemmer)

Johannes Markert (together with Prof. Dr. Gassner, Mathematisches Institut)

Tim-Eric Rathjen

Dr. Johanna Malinen

Dr. Juan Ibanez-Mejia

Development of high-resolution techniques for 3D numerical simulations

Implementation of Heating/Cooling Schematics in Gandalf

Numerical simulations of supernova explosions in structured media

ISM turbulent boxes, implementation and analysis of novel high order MHD solvers

High performance computing

Formation of dense molecular clouds in the model of colliding warm atomic flows.

Convergence of chemical species with increasing resolution.

Comparison of different chemical networks.

HPC with the AMR MHD code FLASH

Comparison between simulations and observations:

Post-processing of 3D MHD simulations with radiative transfer codes

(e.g. RADMC-3D) to obtain synthetic emission maps.

So far the study is focussed on synthetic [CII] line emission.

3D simulations of the turbulent interstellar medium, focusing upon the behavior of non-isothermal gas under the influence of driven turbulence.

Andre Klepitko

Radiation pressure on dust and gas

Low-mass star formation

Episodic protostellar outflows

SPH simulations with Gandalf

Development of HII regions in structured media with FLASH

Simulations with the AMR code FLASH

Gas flows in Laval nozzles

Molecule formation in galactic outflows

3D Simulations with Gadget

Michael Weis

MHD simulations of colliding gas flows

Molecular cloud formation

Star formation and ISM


3D MHD simulations, comparing simulated observations with multiwavelength observations

I am using 3D MHD numerical simulations to understand how the interplay between several physical and chemical processes (e.g. turbulence, self-gravity, stellar feedback, magnetic fields, radiative heating and cooling) influences the dynamical evolution of the interstellar medium of galaxies, with a particular interest in the dynamical properties and evolution of molecular clouds.

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Modelling of Supernova explosions in structured media


Feedback processes in molecular clouds


Radiative Feedback implementation