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Disk Dispersal and Planet Formation Time Scales
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Well before the existence of exo-solar systems was confirmed, it was accepted knowledge that most -- if not all -- stars possess circumstellar material during the first one-to-several million years of their pre-main sequence lives, and thus that they commonly have the potential to form planets. Here I summarize current understanding regarding the evolution of proto-planetary dust and gas disks, emphasizing the diversity in evolutionary paths.
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JWST/MIRI Detection of Molecular H$_2$ Winds from an Edge-on Class II Source HV Tau C
The edge-on Class II disk HV Tau C hosts a spatially extended, wide-angled molecular hydrogen wind with warm (~600 K) and hot (~2000 K) components and a mass-loss rate near 1e-8 solar masses per year.
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