Oral Presentation

Constraining MHD Disk Wind Mass Loss Rates from Multiple Molecular Lines: An Application to HH30

Author(s): Sophie Clark (University of Arizona), Uma Gorti (SETI Institute, NASA Ames Research Center), Ilaria Pascucci (University of Arizona), Naman Bajaj (University of Arizona)

Presenter: Sophie Clark (University of Arizona)

Simulations predict that radially extended magnetohydrodynamic (MHD) disk winds may remove sufficient angular momentum from protoplanetary disks to enable accretion, consequently controlling the mass reservoir available for planet formation. Recent JWST observations of HH30's edge-on disk show a narrow cone of H2 emission nested within a wider cone of CO emission; this nested chemical structure is consistent with theoretical predictions of MHD disk winds. In this talk, I will discuss our method of constraining mass loss rates for HH30's disk wind across several emission lines by applying a simple model prescription for MHD disk winds using the emission flux distribution from JWST spectral maps. From this analysis, we find a low wind mass loss rate for the inner disk, implying that most of the mass is removed from the cold, outer region of the disk. Further modeling of other sources will determine how the radial profile of wind mass loss correlates with age and other disk characteristics, which is essential to interpreting the impact of MHD disk winds on accretion.