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Understanding the collapse of clouds and the formation of protoplanetarydisks is essential to understanding the formation of stars and planets. Infalland accretion, the mass-aggregation processes that occur at envelope and diskscales, drive the dynamical evolution of protostars. While the observations ofprotostars at different stages constrain their evolutionary tracks, the impactof variability due to accretion bursts on dynamical and chemical evolution ofthe source is largely unknown. The lasting effects on protostellar envelopesand disks are tracked through multi-wavelength and time domain observationalcampaigns, requiring deep X-ray, infrared, and radio imaging and spectroscopy,at a sufficient level of spatial detail to distinguish contributions from thevarious substructures (i.e., envelope from disk from star from outflow).Protostellar models derived from these campaigns will illuminate the initialchemical state of protoplanetary disks during the epoch of giant planetformation. Insight from individual star formation in the Milky Way is alsonecessary to understand star formation rates in extragalactic sources. Thiscannot be achieved with ground-based observatories and is not covered bycurrently approved instrumentation. Requirements: High (v < 10 km/s for survey;v < 1 km/s for followup) spectral resolution capabilities with relatively rapidresponse times in the IR (3-500 um), X-ray (0.1-10 keV), and radio (cm) arecritical to follow the course of accretion and outflow during an outburst.Complementary, AU-scale radio observations are needed to probe the diskaccretion zone, and 10 AU-scale to probe chemical and kinematic structures ofthe disk-forming regions, and track changes in the dust, ice, and gas withinprotostellar envelopes.

Variability in the Assembly of Protostellar Systems