Sam Geen

TL;DR: In this article, the origin of observed local star formation relations using radiative magnetohydrodynamic simulations with self-consistent star formation and ionising radiation was investigated, and the most diffuse simulated clouds matched the observed clouds relatively well.

TL;DR: In this article, the star formation history of nearby early-type galaxies is investigated via numerical modeling, and it is shown that the evolution of star formation rate is extended over several dynamical times and shows peaks which correspond to pericentre passages of the satellite.

TL;DR: In this article, the yule suite of 26 radiative magnetohydrodynamic (RMHD) simulations of a 10,000 solar mass cloud similar to those in the solar neighbourhood is used to determine how sensitive the star formation efficiency of molecular clouds is to randomised inputs in the star creation feedback loop, and to what extent relationships between emergent cloud properties and the SFE can be recovered.

TL;DR: In this article, a set of radiation-magneto-hydrodynamic simulations of star formation in self-gravitating, turbulent molecular clouds, including their UV radiation feedback, is presented.

TL;DR: In this article, the authors present radiative magnetohydrodynamic simulations of turbulent molecular clouds that form individual stars of 30, 60 and 120 solar masses emitting winds and ultraviolet radiation following realistic stellar evolution tracks.