REVIEW 16 cited by
Setting the Stage for Planet Formation: Measurements and Implications of the Fundamental Disk Properties
Not yet reviewed by Pith; the record is open.
This paper has not been read by Pith yet. Machine review is queued; the pith claim, tier, and objections will appear here once it completes.
SPECIMEN: schema-true, not a live event
T0 review · schema-true
One-sentence machine reading of the paper's core claim.
pith:XXXXXXXX · record.json · timestamp
read the original abstract
The field of planet formation is in an exciting era, where recent observations of disks around low- to intermediate-mass stars made with state of the art interferometers and high-contrast optical and IR facilities have revealed a diversity of substructures, some possibly planet-related. It is therefore important to understand the physical and chemical nature of the protoplanetary building blocks, as well as their spatial distribution, to better understand planet formation. Since PPVI, the field has seen tremendous improvements in observational capabilities, enabling both surveys of large samples of disks and high resolution imaging studies of a few bright disks. Improvements in data quality and sample size have, however, opened up many fundamental questions about properties such as the mass budget of disks, its spatial distribution, and its radial extent. Moreover, the vertical structure of disks has been studied in greater detail with spatially resolved observations, providing new insights on vertical layering and temperature stratification, yet also bringing rise to questions about other properties, such as material transport and viscosity. Each one of these properties - disk mass, surface density distribution, outer radius, vertical extent, temperature structure, and transport - is of fundamental interest as they collectively set the stage for disk evolution and corresponding planet formation theories. In this chapter, we will review our understanding of the fundamental properties of disks including the relevant observational techniques to probe their nature, modelling methods, and the respective caveats. Finally, we discuss the implications for theories of disk evolution and planet formation underlining what new questions have since arisen as our observational facilities have improved.
Forward citations
Cited by 16 Pith papers
-
The ALMA Survey of Gas Evolution of PROtoplanetary Disks (AGE-PRO): I. Program Overview and Summary of First Results
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...
-
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.
-
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.
-
A portrait throughout perihelion of the NH$_2$-rich interstellar comet 2I/Borisov
2I/Borisov is confirmed as carbon-depleted and NH2-rich among measured comets, with a significant rise in NH2 production after its 2020 splitting event.
-
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.
-
The ALMA Survey of Gas Evolution of PROtoplanetary Disks (AGE-PRO): XII. Extreme millimetre variability detected in a Class II disc
ALMA caught the Class II disk J16202 flaring at 1.3 mm, fading by a factor of 8 in under an hour; the emission is likely non-thermal synchrotron from near the star.
-
The ALMA Survey of Gas Evolution of PROtoplanetary Disks (AGE-PRO): X. Dust Substructures, Disk Geometries, and Dust-disk Radii
Analysis of 30 protoplanetary disks finds dust substructures in about 80% of resolved young Class I disks and a rising fraction of large inner dust cavities in older regions, suggesting early and efficient planet formation.
-
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.
-
The ALMA Survey of Gas Evolution of PROtoplanetary Disks (AGE-PRO): V. Protoplanetary gas disk masses
Median protoplanetary disk gas mass falls from about 0.007 solar masses in Ophiuchus (under 1 Myr) to about 0.0007 to 0.0009 solar masses in Lupus and Upper Sco (1 to 6 Myr), with carbon monoxide depleted about tenfol...
-
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.
-
Characterizing the oxidation state of rocky exoplanets with the Large Interferometer for Exoplanets (LIFE)
LIFE baseline mid-IR observations of Earth-sized planets at 10 pc can retrieve CO2, CH4, and NH3 well enough to distinguish mantle redox states from IW-6 to IW+6 under the paper's modeling assumptions.
-
Extending dynamical mass measurements: probing GI as a possible origin of mm-dust spirals
Dynamical rotation-curve fits give M_disk ≈ 0.30 M_sun for HD 97048 and ≈ 0.21 M_sun for WaOph 6, and indicate disks with mm-dust spirals have systematically lower Toomre Q.
-
Ionized gas emission in protoplanetary disks with the SKAO
Synthetic SKA-Mid observations of simulated MHD and photoevaporative disk winds show that free-free emission is detectable in hours and stacked hydrogen recombination lines are spectrally resolvable in ~10 hours.
-
Connecting Planetary Composition with Formation: a New Paradigm Emerges
A synthesis review argues that MHD disk winds, not turbulence, dominate disk evolution and planet formation, linking observed disk structures to exoplanet composition and orbits.
-
On Linking Planet Formation Models, Protoplanetary Disk Properties, and Mature Gas Giant Exoplanet Atmospheres
A workshop synthesis concludes that linking gas giant exoplanet atmospheres to formation histories requires multiple elemental abundance tracers, not a single C/O ratio, and identifies the most pressing open questions.
-
An Introduction to Dust Evolution and Vertical Transport in Protoplanetary Disks
A tutorial that reviews the physics and observational methods for measuring dust sizes and vertical settling in protoplanetary disks.
Discussion (0). Sign in to comment.