Star formation

Most of my work on star formation involves trying to connect the predictions of theoretical models to what actually gets observed by telescopes, primarily molecular line emission. Synthetic observations, the result of combining hydrodynamics, chemistry and radiative transfer, can be compared directly with observational data. This is much easier than trying to use the data to work out the underlying physical properties of whatever is being observed. The aim is to extract hard predictions from the various competing theories of star formation: if x happens, then the molecular line data should look like y. Quite frequently, they don’t.

Simulated cloud seen in HCN emission

Dust, supernovae, dusty supernovae

Core-collapse supernovae are known to produce large masses of dust. However, it is commonly held that this still isn’t enough to explain the observed dust masses in galaxies, particularly as supernovae also destroy dust, and therefore additional dust formation in the interstellar medium is required. My work on this is split into two parts: using infrared observations of supernova remnants to tie down some of the many unknowns going into models of dust evolution; and reevaluating the underlying assumptions made by these models, which often neglect important physical processes. The results suggest a much more supernova-friendly picture of where all the dust comes from.