REVIEW 12 cited by
Disk Frequencies and Lifetimes in Young Clusters
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
We report the results of the first sensitive L-band (3.5 micron) survey of the intermediate age (2.5 - 30 Myr) clusters NGC 2264, NGC 2362 and NGC 1960. We use JHKL colors to obtain a census of the circumstellar disk fractions in each cluster. We find disk fractions of 52% +/- 10%, 12% +/- 4% and 3% +/- 3% for the three clusters respectively. Together with our previously published JHKL investigations of the younger NGC 2024, Trapezium and IC 348 clusters, we have completed the first systematic and homogenous survey for circumstellar disks in a sample of young clusters that both span a significant range in age (0.3 - 30 Myr) and contain statistically significant numbers of stars whose masses span nearly the entire stellar mass spectrum. Analysis of the combined survey indicates that the cluster disk fraction is initially very high (> 80%) and rapidly decreases with increasing cluster age, such that half the stars within the clusters lose their disks in < ~3 Myr. Moreover, these observations yield an overall disk lifetime of ~ 6 Myr in the surveyed cluster sample. This is the timescale for essentially all the stars in a cluster to lose their disks. This should set a meaningful constraint for the planet building timescale in stellar clusters. The implications of these results for current theories of planet formation are briefly discussed.
Forward citations
Cited by 12 Pith papers
-
Dust transport in envelopes of disk-embedded planets: I. Convectively stable envelopes
In convectively stable envelopes of embedded Earth-like planets, the dust-to-gas ratio falls by 2 to 4 orders of magnitude toward the core, because small grains are blocked by the recycling flow and large grains settl...
-
Dust transport in envelopes of disk-embedded planets: II. Fully convective envelopes
In fully convective envelopes of disk-embedded planets, dust is retained only when convection reaches the disk flow and grains are small enough to be trapped by convective stirring.
-
Beyond Point Masses. VI. Spin-Orbit Evolution of the Centaur Binary Typhon-Echidna
The mutual orbit of Typhon-Echidna is precessing rapidly, revealing Typhon's J2, a 24 degree spin-orbit misalignment, and a triaxial shape consistent with a recently excited binary.
-
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.
-
LBT-MODS spectroscopy of young stellar objects in the distant metal-poor star forming region Sh2-284: Stellar and accretion properties
In the metal-poor region Sh2-284, disk-bearing young stars accrete at a median rate of ~2.2e-8 Msun/yr, comparable to solar-metallicity regions, with tentative evidence that accretion-tracer flux relations flatten at ...
-
The majority of hot Jupiters formed beyond the water ice line
At least six of nine hot Jupiters are consistent with forming beyond the water ice line, implying inward migration with dynamical scattering for many of them.
-
How to measure tidal dissipation in long resonant chains
A matrix-based extension of Papaloizou (2015) gives the tidal separation timescale T for N-planet chains and converts observed offsets into effective Q' bounds, with special sensitivity to the second and outermost pla...
-
Planet formation at the inner edge of the dead zone II. Outbursts, rings, vortices, and suppression of planetesimal formation
2D radiation-hydrodynamical simulations find accretion outbursts unstable to Rossby-wave instability, forming vortices that suppress planetesimal formation until post-burst quiescence.
-
Scattered light signatures of flyby-induced warps in protoplanetary discs
Flyby-induced warps create observable oscillating shadows in scattered light for low-viscosity discs lasting most of their ~10^6 year lifetime, enabling surveys to probe viscosity.
-
Dynamical formation of long-period exoplanets systems in evolving binary stars
MESA+REBOUND simulations show that stellar mass loss in a wide binary destabilizes S-type multi-planet systems and pushes surviving giants to long-period orbits.
-
CHEOPS observations of V1298 Tau: updated planetary densities and implications on the early evolution of the young system
CHEOPS photometry improves radii for V1298 Tau b, c, and d, producing revised densities of 0.06-0.23 g cm^{-3} that indicate differential atmospheric evolution and no requirement for past dynamical excitation.
-
The Natural History of 'Oumuamua
A review finds all available observations of 'Oumuamua consistent with natural processes from Solar System minor bodies and planetary evolution.
Discussion (0). Continue with ORCID to comment.