Determining Dispersal Mechanisms of Protoplanetary Disks Using Accretion and Wind Mass Loss Rates
AffiliationSteward Observatory, Department of Astronomy, University of Arizona
Lunar and Planetary Laboratory, University of Arizona
MetadataShow full item record
PublisherAmerican Astronomical Society
CitationHasegawa, Y., Haworth, T. J., Hoadley, K., Kim, J. S., Goto, H., Juzikenaite, A., Turner, N. J., Pascucci, I., & Hamden, E. T. (2022). Determining Dispersal Mechanisms of Protoplanetary Disks Using Accretion and Wind Mass Loss Rates. Astrophysical Journal Letters.
JournalAstrophysical Journal Letters
RightsCopyright © 2022. The Author(s). Published by the American Astronomical Society. Original content from this work may be used under the terms of the Creative Commons Attribution 4.0 licence.
Collection InformationThis item from the UA Faculty Publications collection is made available by the University of Arizona with support from the University of Arizona Libraries. If you have questions, please contact us at email@example.com.
AbstractUnderstanding the origin of accretion and dispersal of protoplanetary disks is fundamental for investigating planet formation. Recent numerical simulations show that launching winds are unavoidable when disks undergo magnetically driven accretion and/or are exposed to external UV radiation. Observations also hint that disk winds are common. We explore how the resulting wind mass loss rate can be used as a probe of both disk accretion and dispersal. As a proof-of-concept study, we focus on magnetocentrifugal winds, magnetorotational instability turbulence, and external photoevapotaion. By developing a simple yet physically motivated disk model and coupling it with simulation results available in the literature, we compute the wind mass loss rate as a function of external UV flux for each mechanism. We find that different mechanisms lead to different levels of mass loss rate, indicating that the origin of disk accretion and dispersal can be determined, by observing the wind mass loss rate resulting from each mechanism. This determination provides important implications for planet formation. This work thus shows that the ongoing and future observations of the wind mass loss rate for protoplanetary disks are paramount to reliably constrain how protoplanetary disks evolve with time and how planet formation takes place in the disks. © 2022. The Author(s). Published by the American Astronomical Society.
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VersionFinal published version
Except where otherwise noted, this item's license is described as Copyright © 2022. The Author(s). Published by the American Astronomical Society. Original content from this work may be used under the terms of the Creative Commons Attribution 4.0 licence.