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Accretion streamers, protoplanetary disk, and outflow in the Class I source Oph IRS63

Abstract

The widespread detection of rings and gaps around T Tauri stars' disks suggests that planet formation may actually start during the protostellar phase. However, unlike T Tauri stars, protostars are still surrounded by dense envelopes of gas and dust. These envelopes can interact with the disks, altering the disk's dynamics, chemistry, and amount of material available for planet formation. Oph IRS63 is one of the youngest protostars with confirmed annular structures in its dust disk, which suggests that planet formation may already be underway. In this talk, I present the first high-resolution observations of the gas environment around Oph IRS63 as part of the eDisk Large ALMA program. This protostar exhibits a shell-like bipolar outflow, streamers connecting a large rotating envelope to the disk, and several small-scale spirals seen toward the edge of the dust continuum. Additionally, I describe the dynamic nature of these large-scale structures and how the mass transfer from the envelope to the disk leads to a mass build-up phase, which could result in disk instabilities.