Hydrodynamic Photoevaporation of Protoplanetary Disks with Consistent Thermochemistry

Wang, Lile; Goodman, Jeremy

doi:10.3847/1538-4357/aa8726

Cited by 75 publications

(98 citation statements)

References 55 publications

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“…Here we find that the advection timescale is significantly exceeding the timescale for the recombination processes. This result stands in contrast to Wang & Goodman (2017) who found adiabatic cooling to play an important role for the thermal balance of their models. There are however a number of important differences in the model setup and assumptions which may contribute to these discrepancies.…”

Section: Transition Discscontrasting

confidence: 96%

Radiation-hydrodynamical models of X-ray photoevaporation in carbon-depleted circumstellar discs

Wölfer

Picogna

Ercolano

et al. 2019

Monthly Notices of the Royal Astronomical Society

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The so-called transition discs provide an important tool to probe various mechanisms that might influence the evolution of protoplanetary discs and therefore the formation of planetary systems. One of these mechanisms is photoevaporation due to energetic radiation from the central star, which can in principal explain the occurrence of discs with inner cavities like transition discs. Current models, however, fail to reproduce a subset of the observed transition discs, namely objects with large measured cavities and vigorous accretion. For these objects the presence of (multiple) giant planets is often invoked to explain the observations. In our work we explore the possibility of X-ray photoevaporation operating in discs with different gas-phase depletion of carbon and show that the influence of photoevaporation can be extended in such low-metallicity discs. As carbon is one of the main contributors to the X-ray opacity, its depletion leads to larger penetration depths of X-rays in the disc and results in higher gas temperatures and stronger photoevaporative winds. We present radiationhydrodynamical models of discs irradiated by internal X-ray+EUV radiation assuming Carbon gas-phase depletions by factors of 3,10 and 100 and derive realistic mass-loss rates and profiles. Our analysis yields robust temperature prescriptions as well as photoevaporative mass-loss rates and profiles which may be able to explain a larger fraction of the observed diversity of transition discs.

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Section: Transition Discscontrasting

confidence: 96%

Radiation-hydrodynamical models of X-ray photoevaporation in carbon-depleted circumstellar discs

Wölfer

Picogna

Ercolano

et al. 2019

Monthly Notices of the Royal Astronomical Society

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“…Moreover, the overall profile of the PEW profile (i.e., decreasing with radius) is not changed (see Fig. 8 of Wang & Goodman 2017, Σ PEW ∝ r −2 ). Therefore we believe that the the evolutionary nature and the conclusion in this article are not affected by the updated PEW model.…”

Section: Photoevaporation Modelsmentioning

confidence: 96%

“…2.4). Recently there has been much progress on the PEW models by Wang & Goodman (2017) and Nakatani et al (2018a,b). They performed radiation hydrodynamic simulations including X-ray and UV radiation.…”

Section: Photoevaporation Modelsmentioning

confidence: 99%

Dispersal of protoplanetary discs by the combination of magnetically driven and photoevaporative winds

Kunitomo

Suzuki

Inutsuka

2020

Monthly Notices of the Royal Astronomical Society

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We investigate the roles of magnetically driven disk wind (MDW) and thermally driven photoevaporative wind (PEW) in the long-time evolution of protoplanetary disks. We start simulations from the early phase in which the disk mass is 0.118 M around a 1 M star and track the evolution until the disk is completely dispersed. We incorporate the mass loss by PEW and the mass loss and magnetic braking (wind torque) by MDW, in addition to the viscous accretion, viscous heating, and stellar irradiation. We find that MDW and PEW respectively have different roles: magnetically driven wind ejects materials from an inner disk in the early phase, whereas photoevaporation has a dominant role in the late phase in the outer ( 1 au) disk. The disk lifetime, which depends on the combination of MDW, PEW, and viscous accretion, shows a large variation of ∼ 1-20 Myr; the gas is dispersed mainly by the MDW and the PEW in the cases with a low viscosity and the lifetime is sensitive to the mass-loss rate and torque of the MDW, whereas the lifetime is insensitive to these parameters when the viscosity is high. Even in disks with very weak turbulence, the cooperation of MDW and PEW enables the disk dispersal within a few Myr.

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“…Nonetheless, the ability to reproduce the observed line intensities and their approximate profiles is an important requirement for a viable photoevaporation model. One example is the observation of a blue-shift in the [OI] line at 6300Å, which immediately points to a warm quasi-neutral wind, hence ruling out EUV-driven photoevaporation, which produces a fully ionised wind, as in the case of the recent simulations by Wang & Goodman (2017b). In this context, we have calculated here line intensities and line profiles from our new models, via a post-processing of the hydrodynamical grids through the 3D photoionisation and dust radiative transfer code MOCASSIN (Ercolano et al 2003(Ercolano et al , 2005(Ercolano et al , 2008a, and showed that these are in agreement with current observational data.…”

Section: Transition Disc Demographicsmentioning

confidence: 86%

The dispersal of protoplanetary discs – I. A new generation of X-ray photoevaporation models

Picogna

Ercolano

Owen

et al. 2019

Monthly Notices of the Royal Astronomical Society

141

234

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Photoevaporation of planet-forming discs by high energy radiation from the central star is potentially a crucial mechanism for disc evolution and it may play an important role in the formation and evolution of planetary systems. We present here a new generation of X-ray photoevaporation models for solar-type stars, based on hydrodynamical simulations, which account for stellar irradiation via a significantly improved parameterisation of gas temperatures, based on detailed photoionisation and radiation transfer calculations. This is the first of a series of papers aiming at providing a library of models which cover the observed parameter space in stellar and disc mass, metallicity and stellar X-ray properties. We focus here on solar-type stars (0.7 M ) with relatively low-mass discs (1% of the stellar mass) and explore the dependence of the wind mass-loss rates on stellar X-ray luminosity. We model primordial discs and transition discs at various stages of evolution. Our 2D hydrodynamical models are then used to derive simple recipes for the mass-loss rates that are suitable for one-dimensional disc evolution and/or planet formation models typically employed for population synthesis studies. Line profiles from typical wind diagnostics ([OI] 6300Å and [NeII] 12.8 µm) are also calculated for our models and found to be roughly in agreement with previous studies. Finally, we perform a population study of transition discs by means of one-dimensional viscous evolution models including our new photoevaporation prescription and find that roughly a half of observed transition discs cavities and accretion rates could be reproduced by our models.

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Hydrodynamic Photoevaporation of Protoplanetary Disks with Consistent Thermochemistry

Cited by 75 publications

References 55 publications

Radiation-hydrodynamical models of X-ray photoevaporation in carbon-depleted circumstellar discs

Radiation-hydrodynamical models of X-ray photoevaporation in carbon-depleted circumstellar discs

Dispersal of protoplanetary discs by the combination of magnetically driven and photoevaporative winds

The dispersal of protoplanetary discs – I. A new generation of X-ray photoevaporation models

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