Dust dynamics during protoplanetary disc clearing

By Richard Alexander, Philip Armitage. 2007

164 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Spectroscopy

View Paper: https://www.semanticscholar.org/paper/32c4801f16e83b6007b88c34ad354da858feef87

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Citations in the corpus

DUST FILTRATION BY PLANET-INDUCED GAP EDGES: IMPLICATIONS FOR TRANSITIONAL DISKS (2012, background): “Thus it’s possible to explain pre-transitional disks without invoking dust growth (e.g. dust filtration, multiple-planets, photoevaporation Alexander & Armitage 2007).”
Observational Signatures of Planets in Protoplanetary Disks I: Gaps Opened by Single and Multiple Young Planets in Disks (2014, background): “…mechanisms can partially explain the observations, including grain growth (Dullemond & Dominik 2005; Birnstiel et al. 2012), photoevaporation (Alexander & Armitage 2007, 2009; Owen et al. 2012; Rosotti et al. 2013), infall from counterrotating external environments (Vorobyov et al. 2014),…”
A SPATIALLY RESOLVED INNER HOLE IN THE DISK AROUND GM AURIGAE (2009, background): “As noted by Alexander & Armitage (2007), the properties of the GM Aur system are inconsistent with a photoevaporative scenario because the large mass of the outer disk should still be sufficient to provide a substantial accretion rate to counteract the photoevaporative wind.”
TRANSITIONAL AND PRE-TRANSITIONAL DISKS: GAP OPENING BY MULTIPLE PLANETS? (2010, background): “Photoevaporation has been proposed as one gap/hole clearing mechanism (Alexander & Armitage 2007, 2009), but requires the mass loss rate by the photoevaporation to be comparable to the disk accretion rate.”
The Growth Mechanisms of Macroscopic Bodies in Protoplanetary Disks (2008, background): “Photoevaporation by stellar radiation, stellar winds, giant planets, or photophoresis has been suggested to eventually clear the inner disk (Alexander & Armitage 2007; Takeuchi, Miyama & Lin 1996; Krauss et al. 2007), whereas photoevaporation by nearby massive stars might destroy the outer disk…”
UNVEILING THE STRUCTURE OF PRE-TRANSITIONAL DISKS (2010, background): “Once the isolated inner disk drains onto the star on the viscous timescale, the inner edge of the outer disk will be directly irradiated by the star and the hole will keep growing outward (Alexander & Armitage 2007).”
PARTICLE CLUMPING AND PLANETESIMAL FORMATION DEPEND STRONGLY ON METALLICITY (2009, background): “For example, photoevaporation removes gas from the disk surface, leaving behind larger solids that have sedimented to the mid-plane (Throop & Bally 2005; Alexander & Armitage 2007).”
TRANSITIONAL DISKS AS SIGNPOSTS OF YOUNG, MULTIPLANET SYSTEMS (2011, background): “Prior work on UV photoevaporation showed that evaporation-induced inner holes were inconsistent with accretion rates higher than∼ 10−10M⊙ yr −1 (Alexander & Armitage 2007).”
Protoplanetary disc evolution and dispersal: the implications of X-ray photoevaporation (2010, background): “Alexander & Armitage (2007) examined the behaviour of dust in a photoevaporating disc, finding that, under the action of dust drag, the time-scale for dust grains c© 2002 RAS, MNRAS 000, 1–15 to drain onto the star is of order 103yrs, after the gap opens, approximately two order of magnitudes…”
Small vs. large dust grains in transitional disks: do different cavity sizes indicate a planet? - SAO 206462 (HD 135344B) in polarized light with VLT/NACO (2013, background): “Alexander & Armitage (2007) argued that UV photoevaporation can induce holes only in systems with accretion rates.”
GIANT PLANET MIGRATION, DISK EVOLUTION, AND THE ORIGIN OF TRANSITIONAL DISKS (2009, methodology): “We setΣc = 10−5g cm−2, but note that the results are not very sensitive to the exact value adopted (see discussion in Alexander & Armitage 2007).”
Prograde rotation of protoplanets by accretion of pebbles in a gaseous environment (2009, background): “The evaporation of gas by irradiation from the central star or neighbouring O stars leads to a similar increase in the influence of the dust particles on the gas (Throop & Bally 2005; Alexander & Armitage 2007; Johansen, Youdin, & Mac Low 2009).”
PROTOPLANETARY DISK STRUCTURES IN OPHIUCHUS (2009, background): “Toward the end of the disk lifetime, winds driven by energetic radiation from the central star can rapidly sweep any remaining material into the local environment (Clarke et al. 2001; Alexander et al. 2006; Alexander & Armitage 2007).”
Spectroastrometric Imaging of Molecular Gas within Protoplanetary Disk Gaps (2008, background): “Photo-evaporation will create holes in the radial gas and dust distribution extending all the way to the stellar surface, if the disk is not too massive (Alexander & Armitage 2007).”
EVIDENCE FOR DUST CLEARING THROUGH RESOLVED SUBMILLIMETER IMAGING (2008, background): “For planetary companions of sufficient mass, some disk gas is expected to be transported across the gap while the dust transport is strongly inhibited (Alexander & Armitage 2007).”
PROTOPLANETARY DISK STRUCTURES IN OPHIUCHUS. II. EXTENSION TO FAINTER SOURCES (2010, background): “Alternatively, they may represent a true lack of material in the inner disk, cleared out by a photoevaporative wind and viscous draining (Alexander & Armitage 2007) or tidal interactions with faint companions - perhaps even young planetary systems (e.g., Lubow & D’Angelo 2006).”
RESOLVED IMAGES OF LARGE CAVITIES IN PROTOPLANETARY TRANSITION DISKS (2011, background): “Najita et al. (2007) suggested that transition disks exhibit low accretion rates compared to their normal counterparts with similar disk masses, consistent with a large reduction in the mass flow across a gap produced by a low-mass companion (see also Alexander & Armitage 2007, 2009).”