Using chemistry to trace protostellar mass accretion
Author: Soren Frimann
Understanding how stars gain their mass is a fundamental question of star formation with consequences for both the physical and chemical evolution of young stellar systems. In particular, is the mass accretion onto young stars smooth with time or is it better characterised by short episodic bursts of high accretion? There is increased evidence that mass accretion onto young stars is episodic, but bursts are rare and therefore difficult to observe directly. In the talk, I will present results from a novel method whereby chemistry can be used to observe the effects of an accretion bursts thousands of years after the burst itself has ended.