Milky Way Analogue Isolated Disk Galaxy
From Jeffrey Carpenter
Funded in part by: National Science Foundation Award: ACI-1445176
The Centrality of Advance Dgitally Enabled Science: CADENS
The properties of disk galaxies are determined by a balance between self-gravity, angular momentum, and "feedback" from the supernova explosions produced by young, massive stars. Gravity causes gas in the interstellar medium to condense and collapse, forming new generations of stars. After only a few million years, supernova explosions produced by the most massive newborn stars in turn disrupt their natal star forming regions, preventing further star formation and redistributing gas from lower densities. Later, the gas recondenses, and collapses forming another generation of stars. This ongoing cycle of stellar collapse, birth, death, and rarefacation proceeds for billions of years, until the gas supply is slowly exhausted. This movie shows the evolution of a simulated analogue for the Milky Way galaxy over the course of 50 million years.
This work was supported by NSF graduate fellowships (NJG and JCF), by NSF grants AST-0955300, AST-1405962 (MRK, NJG, and JCF), and ACI-1535651 (NJG), by NASA TCAN grant NNX14AB52G (MRK, NJG, and JCF), by Hubble Archival Research grant HST-AR-13909 (JCF and MRK), by grant DP16010100695 from the Australian Research Council (MRK), and by the Gordon and Betty Moore Foundationʼs Data-Driven Discovery Initiative through Grant GBMF4651 to Matthew Turk.
(In this context, NJG is Nathan Goldbaum, JCF is John Forbes, and MRK is Mark Krumholz.)
COMPUTED AT: Pleiades @ NASA Ames, Hyades cluster @ UCSC
DATA SIZE: 8 TB simulation [we used a 1.8TB subset of that]
DATA RESOLUTION: 10 AMR levels (finest scale is 2 parsecs)
SPATIAL SCALE: 50,000 parsecs (size of galaxy within 1.3 megaparsec simulation)
TIME SCALE: 50 million years, in 50,000-year timesteps