Photoevaporation of protoplanetary discs – I. Hydrodynamic models

By Richard Alexander, C. Clarke, J. E. Pringle. 2006

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In this paper we consider the effect of the direct ionizing stellar radiation field on the evol ution of protoplanetary discs subject to photoevaporative winds. We suggest that models which combine viscous evolution with photoevaporation of the disc (e.g. Clarke, Gendrin & Sotomayor 2001) incorrectly neglect the direct field after the inner disc has drained, at late times in the evolution. We construct models of the photoevaporative wind produced by the direct field, first using simple analytic arguments and later using d etailed numerical hydrodynamics. We find that the wind produced by the direct field at late times i s much larger than has previously been assumed, and we show that the mass-loss rate scales as R 1/2 in (where Rin is the radius of the instantaneous inner disc edge). We suggest that this result has important consequences for theories of disc evolution, and go on to consider the effects of this result on disc evolution in detail in a companion paper (Alexander, Clarke & Pringle 2006).

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/d820d5034da5636173a2273df1fe112811f97165

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Protoplanetary Disks and Their Evolution (2011, background): “However, according to the “UV-switch” model (Alexander et al., 2006), photoevaporation removes all circumstellar gas very quickly (≪ 1Myr) once accretion stops (see §6.2).”
Radiation-hydrodynamic models of X-ray and EUV photoevaporating protoplanetary discs (2009, methodology): “However a more detailed approach will be required when it comes to predicting the statistical distribution of inner hole sizes as a function of stellar parameters (Alexander et al. 2006b).”
RESOLVED IMAGES OF LARGE CAVITIES IN PROTOPLANETARY TRANSITION DISKS (2011, background): “…to explain observations of transition disks, including extensive particle growth (Tanaka et al. 2005; Dullemond & Dominik 2005), photoevaporative massloss in winds (Clarke et al. 2001; Alexander et al. 2006a), and tidal interactions with companions (e.g., Rice et al. 2003a; Ireland & Kraus 2008).”
Dust dynamics during protoplanetary disc clearing (2007, methodology): “Our models show that the dust-to-gas ratios for small grains are approximately constant (away from the edge of the gas disc), so our predictions regarding near-and midinfrared emission agree well with previous gas-only models (e.g. Alexander et al. 2006b).”
The Spitzer Survey of the Small Magellanic Cloud: S3MC Imaging and Photometry in the Mid- and Far-Infrared Wave Bands (2006, background): “Models of less massive stars, however, suggest that the outer disk clearing time is dominated by photoevaporation and that its dispersal occurs very quickly after the inner disk is cleared (Alexander et al. 2006a, 2006b).”
PHOTOEVAPORATION OF CIRCUMSTELLAR DISKS BY FAR-ULTRAVIOLET, EXTREME-ULTRAVIOLET AND X-RAY RADIATION FROM THE CENTRAL STAR (2008, background): “EUV, FUV, and X-ray photons now directly impact the newly formed rim and the outer disk is subsequently rapidly eroded ( 105 yr) from inside out (as discussed in Alexander et al. 2006b).”
GIANT PLANET MIGRATION, DISK EVOLUTION, AND THE ORIGIN OF TRANSITIONAL DISKS (2009, background): “…distributions: planets (Rice et al. 2003; Quillen et al. 2004), dust evolution (Dullemond & Dominik 2005; Krauss et al. 2007), disk clearing (Alexander et al. 2006b; Chiang & Murray-Clay 2007) and the presence of companions (Jensen & Mathieu 1997; Ireland & Kraus 2008) probably all play a…”
Survival of molecular gas in cavities of transition disks - I. CO (2013, background): “Photoevaporation (e.g. Bally & Scoville 1982; Hollenbach et al. 1994; Clarke et al. 2001; Alexander et al. 2006; Ercolano et al. 2008; Gorti & Hollenbach 2009) has short processing time-scales and once its effect sets in, would quickly lead to a gas free cavity.”
STRUCTURE AND EVOLUTION OF PRE-MAIN-SEQUENCE CIRCUMSTELLAR DISKS (2009, background): “Until now, photoevaporation, the presence 12 of a planet, grain growth and inside-out MRI clearing have been the main processes invoked to explain the properties of transitional disks (Alexander et al. 2006; Calvet 2005; Espaillat et al. 2008; Dullemond & Dominik 2005; Chiang & Murray-Clay 2007).”
TRANSITIONAL DISKS AS SIGNPOSTS OF YOUNG, MULTIPLANET SYSTEMS (2011, background): “Once the inner disk has become optically thin to Lyman continuum radiation, the direct UV field also drives a photoevaporative wind that drains the outer disk (Alexander et al. 2006a).”
The Sun in Time: Activity and Environment (2007, background): “Disk irradiation and photoionization by stellar UV photons is further responsible for photoevaporation of gaseous disks (Hollenbach et al., 1994; Clarke et al., 2001; Alexander et al., 2006a,b), and therefore the long-term accretion history of the star-disk system.”
Protoplanetary disc evolution and dispersal: the implications of X-ray photoevaporation (2010, methodology): “…(Krauss et al 2007), MRI-driven winds (Suzuki & Inutsuka 2009), and photoevaporation due to extreme ultraviolet radiation -EUV- (Clarke et al 2001; Alexander et al 2006a,b; Richling & Yorke 2000), X-ray radiation (Alexander et al. 2004; Ercolano et al 2008b, 2009; Gorti & Hollenbach 2009, Owen et…”
How to form planetesimals from mm-sized chondrules and chondrule aggregates (2015, background): “The second way to increase Z is to remove gas from the disk, either through late-stage photoevaporation (e.g., Alexander et al. 2006a,b) or through disk winds (Bai & Stone 2013; Suzuki & Inutsuka 2009).”
On the theory of disc photoevaporation (2011, methodology): “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.”