The Griffin project

Galaxy Realizations Including Feedback From INdividual massive stars


Here's what makes GRIFFIN special

Hydro solver

GRIFFIN is using a modern Smoothed Particle Hydrodynamics solver (SPHGal, Hu et al. 2014) as well as the meshless finite mass (MFM) method (Gaburov & Nitadori 2012, Hopkins 2015) as implemented in Steinwandel et al. (2019).

Modeling the interstellar medium

Heating, cooling and the formation/destruction of molecular H2 and CO is modelled with a non-equilibrium chemical network (Nelson & Langer 1997, Glover & Mac Low 2007).

Modeling star formation and feedback

GRIFFIN simulations are run at high (solar mass) mass and spatial (sub-parsec) resolution. Individual massive stars are realised as fundamental indivisable units with their respective evolutionary tracks. We also resolve their energy injection by individual supernovae up to high environmental densities.


The simulations include an interstellar ultraviolet radiation field varying in space and time, with simple implementations for dust and gas shielding and a Strömgren model for photoionization.


The simulation products are carefully post-processed using various open-source analysis tools such as PYGAD (Röttgers et al. 2020).


The simulations are carried out at the MPA cluster Freya, a HPC system hosted by the Max-Planck-Computing and Data Facility as well as SuperMUC-NG hosted by the Leibnitz Supercomputing Centre under the grant pn72bu.


For questions send an email to naab(at)