ALMA Studies of Eruptive Stars

It is now believed that stars acquire most of their mass in short episodes of accretion outbursts. This episodic accretion picture has replaced the traditional steady state accretion model and is changing our understanding on how stars gain their mass (and the origin of the IMF), binary formation, planet formation, the luminosity spread in young clusters, disk chemistry and snowline migration.  Despite its relevance, the physical mechanisms responsible for episodic accretion remain poorly understood. In this poster we present recent observational and modelling advancements aimed at constraining the physical properties of outbursting sources to help understand what drives this important phase of star formation.