The dispersal of circumstellar discs: the role of the ultraviolet switch

By C. Clarke, A. Gendrin, M. Sotomayor. 2001

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View Paper: https://www.semanticscholar.org/paper/b54a8b356ab7d32cc5750150ff8c8d7baeba6ace

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In Astronomy and Astrophysics

Citations in the corpus

A Submillimeter View of Circumstellar Dust Disks in ρ Ophiuchi (2007, background): “Avariety of mechanisms have been proposed for this rapid radial evolution, from planet formation (see Najita et al. 2007 and references therein) to rapid mass loss in photoevaporative winds (Clarke et al. 2001; Alexander et al. 2006).”
Star and Protoplanetary Disk Properties in Orion's Suburbs (2009, background): “…stellar winds, photo-evaporation, or interaction with 2 M. Fang et al.: Star and protoplanetary disk properties in Or on’s suburbs giant gas planets or stellar companions (Artymowicz & Lubow 1994; Clarke et al. 2001; Alexander et al. 2006; Rice et al. 2003; Quillen et al. 2004; Hillenbrand 2008).”
TIME EVOLUTION OF VISCOUS CIRCUMSTELLAR DISKS DUE TO PHOTOEVAPORATION BY FAR-ULTRAVIOLET, EXTREME-ULTRAVIOLET, AND X-RAY RADIATION FROM THE CENTRAL STAR (2009, background): “When EUV photons can remove disk mass at a given radius faster than it can be replenished by viscosity, a gap opens at that radius, as was first noted by Clarke et al. (2001).”
Gas density drops inside dust cavities of transitional disks around young stars observed with ALMA (2015, background): “…of the gas inside the dust hole is essential to distinguish between the possible clearing mechanisms of the dust in the inner part of disk: photoevaporation (Clarke et al. 2001), grain growth (Dullemond & Dominik 2005), clearing by (sub)stellar or planetary companions (e.g. Lin & Papaloizou 1979).”
On the theory of disc photoevaporation (2011, background): “However, in order to be consistent with the previous EUV-only literature (Hollenbach et al. 1994; Clarke et al. 2001; Font et al. 2004; Alexander et al. 2006a), we separately fix Rg = 8.9(1/1 M ) au.”
Accretion onto Pre-Main-Sequence Stars (2016, background): “Simple viscous accretion is unlikely to explain these rapid turn-offs of accretion (Clarke et al. 2001).”
Planet Formation around Stars of Various Masses: The Snow Line and the Frequency of Giant Planets (2007, background): “The short timescale for disk removal by the central star—inferred from the lack of transition disks (e.g. Kenyon & Hartmann 1995; Clarke et al. 2001; Alexander et al. 2006)—and the likely large radial distance in the disk for external influence by massive stars (Adams et al. 2004), supports our…”
EVIDENCE FOR DUST CLEARING THROUGH RESOLVED SUBMILLIMETER IMAGING (2008, background): “One proposed process for quickly clearing the inner disk region is photoevaporation (Clarke et al. 2001, Alexander et al. 2006).”
Dynamical Outcomes of Planet-Planet Scattering (2007, background): “Clarke et al. (2001) proposed that, once the viscous accretion rate drops to a level comparable to the wind mass loss rate, photoevaporation takes over the disk evolution.”
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).”
PHOTOEVAPORATION OF CIRCUMSTELLAR DISKS BY FAR-ULTRAVIOLET, EXTREME-ULTRAVIOLET AND X-RAY RADIATION FROM THE CENTRAL STAR (2008, background): “For EUV photoevaporation which peaks at r ∼ rg,II (Figure 2), when accretion rates in the disk decline to low enough values, a gap forms at r ∼ rg,II and thereafter the outer disk evaporates from inside out (Clarke et al. 2001; Alexander et al. 2006b).”
The Evolution of Gravitationally Unstable Protoplanetary Disks: Fragmentation and Possible Giant Planet Formation (2003, background): “Other solutions, such as photoevaporative flows (Clarke et al. 2001; Armitage et al. 2003), require an input from external irradiation sources, since the heat generated by internal star-disk accretion shocks is probably insufficient (Matsuyama et al. 2003), but this would not work in, for example,…”