Photoevaporation of protoplanetary discs - II. Evolutionary models and observable properties

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

385 citations recorded by the source corpus.

We present a new model for protoplanetary disc evolution. This model combines viscous evolution with photoevaporation of the disc. However, in a companion paper we have shown that at late times such models must consider the effect of stellar radiation directly incident on the inner disc edge, and here we model the observational implications of this process. We find that the entire disc is dispersed on a time-scale of the order of 10 5 yr after a disc lifetime of a few Myr, consistent with observations of T Tauri (TT) stars. We use a simple prescription to model the spectral energy distribution of the evolving disc, and demonstrate that the model is consistent with observational data across a wide range of wavelengths. We also note that the model predicts a short ‘inner hole’ phase in the evolution of all TT discs, and make predictions for future observations at mid-infrared and millimetre wavelengths.

Subfields: Astronomy and Astrophysics, Spectroscopy

View Paper: https://www.semanticscholar.org/paper/a16202c21ea493cb6892777120286fdb6955e316

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Citations in the corpus

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).”
Dynamical Outcomes of Planet-Planet Scattering (2007, methodology): “Alexander et al. (2006) showed that the disk clearing by this mechanism takes about 105 yr, which is comparable to the observed dissipation time.”
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).”
Cold Disks: Spitzer Spectroscopy of Disks around Young Stars with Large Gaps (2007, background): “Do disks clear uniformly throughout via grain growth and settling, or is the process accelerated in the inner regions forming gaps (e.g., Alexander et al. 2006)?”
An ALMA Survey of Protoplanetary Disks in the σ Orionis Cluster (2017, background): “…that viscous disks evolve rapidly into debris disks once stellar accretion ceases and photoevaporation from the central star dominates, clearing the dust from the inside out and leaving behind larger solids such as pebbles and planetesimals (e.g., Clarke et al. 2001; Alexander et al. 2006).”
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).”
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).”
HOW THERMAL EVOLUTION AND MASS-LOSS SCULPT POPULATIONS OF SUPER-EARTHS AND SUB-NEPTUNES: APPLICATION TO THE KEPLER-11 SYSTEM AND BEYOND (2012, background): “Meanwhile, planet formation ends and mass loss becomes important after a few Myr (Calvet et al. 2002; Alexander et al. 2006).”
THE ROLE OF MULTIPLICITY IN DISK EVOLUTION AND PLANET FORMATION (2011, background): “For example, typical circumstellar disks seem to be affected by photoevaporation only at late stages of their evolution, after most of their mass has been accreted to the central star (e.g., Alexander & Armitage 2009; Alexander et al. 2006).”
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).”
The Spitzer c2d Survey of Weak-Line T Tauri Stars. II. New Constraints on the Timescale for Planet Building (2007, background): “Such scenarios include the ultraviolet-switch model (Alexander et al. 2006) and the presence of gap forming planets (e.g. Quillen et al. 2004).”
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.”
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).”
Origins of Eccentric Extrasolar Planets: Testing the Planet-Planet Scattering Model (2007, background): “Since the photoevaporation timescale (∼ 105 yr; Alexander et al. 2006) is often much shorter than the timescale for dynamical instabilities to arise, the outcome of the instabilities are expected to be insensitive to the details of the photoevaporation process.”
The warm gas atmosphere of the HD 100546 disk seen by Herschel - Evidence of a gas-rich, carbon-poor atmosphere? (2012, background): “Appendices A and B are available in electronic form at http://www.aanda.org upper atmosphere, a disk-wind is driven, which may eventually disperse the disk (Alexander et al. 2006; Ercolano et al. 2008; Gorti & Hollenbach 2009).”