Astrophysical Computing

Our Mission: Making Galaxies; One star at a time.
First Stars: About 100 million years after the Big Bang, gas collapsed in the first mini-halos to illuminate the universe for the first time since recombination.
First Galaxies: After the formation of primordial massive stars, stars formed in aggregations that were the first galaxies in the universe.
Magnetic Fields in the Early Universe: Magnetic fields are ubiquitous in the present-day universe. How and where did the first magnetic fields form and grow?
Visualization: To explore computational data, ingenious visualization is essential.
Radiative Transfer: Radiative transfer is an inherently difficult computational problem. We attempt to tackle it in an AMR context.
Fine Structure Metal Line Cooling and Chemistry: Code and physics related to atomic and ionic carbon, oxygen and silicon chemistry and cooling.
Enzo: An Eulerian AMR hydrodynamical code that powers most of our calculations.
Reionization and its Observational Consequences: We use N-body and radiative transfer simulations to model the reionization of the universe on scales of hundreds of comoving megaparsecs
Useful scripts: Here you can find useful shell scripts for various tasks.
Merging of Stanford and UCSD Enzo Branches: In June 2009, we will start to merge all of the additions and fixes we have made at Stanford into the UCSD developmental trunk. This workspace will help us organize our thoughts and efforts.

May