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The Role of Disk Winds in the Evolution and Dispersal of Protoplanetary Disks
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The assembly and architecture of planetary systems strongly depend on the physical processes governing the evolution and dispersal of protoplanetary disks. Since Protostars and Planets VI, new observations and theoretical insights favor disk winds as being one of those key processes. This chapter provides a comprehensive review of recent observations probing outflowing gas launched over a range of disk radii for a wide range of evolutionary stages, enabling an empirical understanding of how winds evolve. In parallel, we review theoretical advancements in both magnetohydrodynamic and photoevaporative disk wind models and identify predictions that can be confronted with observations. By linking theory and observations we critically assess the role of disk winds in the evolution and dispersal of protoplanetary disks. Finally, we explore the impact of disk winds on planet formation and evolution and highlight theoretical work, observations, and critical tests for future progress.
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Cited by 11 Pith papers
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JWST/MIRI Reveals the Evolution from Molecular to Atomic Disk Winds
Across 72 protoplanetary disks, JWST shows atomic jets and molecular winds dominate at high accretion rates and give way to predominantly atomic winds as accretion declines.
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First systematic ALMA survey of protoplanetary gas finds median gas disk mass declining from about 6 Jupiter masses in under 1 Myr disks to about 0.5 Jupiter masses by 2 to 6 Myr, with a non-monotonic gas-to-dust rati...
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JWST/MIRI Detection of Molecular H$_2$ Winds from an Edge-on Class II Source HV Tau C
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Preferential alignment of Class 0, Class I protostellar disks in multiple systems across nine nearby molecular clouds
Disks around young stars in binary and higher-order multiple systems are preferentially aligned out to 6000 AU, implying turbulent fragmentation alone cannot explain how most multiples form.
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Protoplanetary Disk Survival Time-scales: A Blind Survey of Young Clusters up to 100 Myr in the Solar Vicinity
Disk fractions in 32 Gaia-selected clusters decline with age at all wavelengths, but the decay is slower at 12 and 22 microns, and long-lived disks are found predominantly around low-mass stars.
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The ALMA Survey of Gas Evolution of PROtoplanetary Disks (AGE-PRO): VIII. The impact of external photoevaporation on disk masses and radii in Upper Scorpius
External photoevaporation at moderate FUV fluxes (2 to 12 G0) truncates Upper Scorpius disks and explains the compact gas sizes seen by AGE-PRO, where pure viscous evolution fails.
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The ALMA Survey of Gas Evolution of PROtoplanetary Disks (AGE-PRO): VII. Testing accretion mechanisms from disk population synthesis
Population synthesis of ALMA disk masses and sizes favors MHD disk-wind-driven accretion over turbulence-driven accretion with photoevaporation.
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The ALMA Survey of Gas Evolution of PROtoplanetary Disks (AGE-PRO): III. Dust and Gas Disk Properties in the Lupus Star-forming Region
Deep ALMA observations of 10 Lupus disks detect rare CO isotopologues and N2H+, revealing correlations between gas and dust fluxes and giving gas-to-dust mass ratios of 10 to 100.
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A multi-wavelength survey of 20 Ophiuchus protostars finds dust masses tens to hundreds of times larger than millimetre-only estimates, if the adopted dust-opacity model is correct.
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Ionized gas emission in protoplanetary disks with the SKAO
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Star formation, stellar evolution, and planets in high-resolution X-ray imaging
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