The role of turbulence for the origin of stellar masses

Interstellar turbulence controls the formation of stars. In this project you will learn how to form stars in a computer. From the simulations we will produce the birth-mass distribution of stars (Initial Mass Function, IMF) and compare it to the observed IMF. By changing the properties of the turbulence we will then study how the IMF depends on the power spectrum of the turbulence.

The main code used for the project is FLASH (see http://flash.uchicago.edu/site/flashcode/), which we'll run on Australian and international supercomputers with hundreds of compute cores. We will use our own developed python codes and modules to extract data from the simulations, make images, movies and construct the IMF for the stars formed in the simulations. This project does not require any special skills; basic programming experience with Python is useful. Please contact Christoph Federrath (christoph.federrath@anu.edu.au) for further details.

Supervisor contact

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