The Evolutionary Tracks for Low to High Mass Star Formation through Variable Accretion Models

Embedded star formation is largely obscured from even the most modern of telescopes therefore computational modelling is used to provide some of the essential information required to fully understand the intrinsic star forming processes. In this thesis, evolutionary models are calculated for protostars and their environments using the hydrodynamic code STELLAR to describe the growing star itself. The code is modified with constant and variable accretion models with the inclusion of episodic bursts to produce stars of final masses of 1 ? 100M?. Luminosity, radius, temperature and mass parameters are tracked throughout the stellar evolution to find potential signature features of each accretion model.

Indications as to why all accretion methods are supported by observation are found and methods of distinguishing between them are suggested. Recent ATLASGAL observations are used to investigate the appropriate methods of statistical comparison between observational and theoretical data. Progress is made toward successful comparisons of theoretical and observational data, with suggestions for clump L/M distribution data analysed using an initial mass function holding the greatest potential for direct com- parisons between the two.