The Galactica database contains results of heavy numerical simulations computed in order to study the problem of star formation, essentially molecular cloud formation, evolution and collapse.
Understanding the dynamical evolution of the interstellar medium (ISM)and its relation to stellar birth is a key challenge in astronomy and astrophysics.The Galactica project aims at providing observers and theorists studying formation and evolution of molecular clouds, their morphological and kinematical characteristics, and the formation of stars in their interior with a set of theoretical tools and a database of models to aid in the analysis and interpretation of current and future observations.
The goal of this database is to give access to observers, or more generally to any scientist working on a related field, to the results of these numerical simulations, which could be useful to help prepare or analyze observations.
Available projects:
Disk populations
This project aims at providing a self-consistent description of disk formation in massive clumps.
Dusty collapses
This project aims at understanding the dynamical decoupling conditions of gas and dust during the protostellar collapse.
FRIG
This project aims at providing a self-consistently description from a 1kpc piece of galaxy to the prestellar cores
Grain evolution collapse
This project aims at providing a description of the dust evolution during the protostellar collapse.
LS
This project aims at modelling self-consistently a 1kpc piece of galaxy including star formation and stellar feedback.
Large scale driving
Study of the effect of large scale driving on the structure of the ISM and star formation in a 1 kpc box.
M51SIM
High resolution simulations of an M51-like interacting galaxy. The project is designed to study GMC statistics in a galactic context.
Massive core
This project aims at providing simulations of the collapse of a massive core of 100 Msun.
ORION
This project aims at providing a self-consistently description of molecular cloud fragmentation and evolution including the prestellar cores and up to the formation of dense fragments inside them (sink particles representing the stars)
