Radiation Hydrodynamics Simulations of Photoevaporation of Protoplanetary Disks by Ultraviolet Radiation: Metallicity Dependence

Nakatani, Riouhei; Hosokawa, Takashi; Yoshida, Naoki; Nomura, Hideko; Kuiper, Rolf

doi:10.3847/1538-4357/aab70b

Cited by 65 publications

(70 citation statements)

References 109 publications

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“…(ii) perform a radiative transfer and thermochemical calculation at each hydrodynamical step (e.g. Wang & Goodman 2017b;Nakatani et al 2018). (iii) Alternatively, an analytic model of the self-similar solution of thermal winds topology has been derived for an isothermal disc (Clarke & Alexander 2016).…”

Section: Methodsmentioning

confidence: 99%

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

140

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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Section: Methodsmentioning

confidence: 99%

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

140

234

View full text Add to dashboard Cite

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“…where 𝑛 H is the number density of hydrogen nuclei, 𝑦 𝑖 = 𝑛 𝑖 /𝑛 H is the fractional abundance of each chemical specie, and 𝑅 𝑖 is the reaction rate of the 𝑖-th specie. We adopt the simple chemical network of Nelson & Langer (1997) for CO formation, which has been used for the RHD simulations (e.g., Hosokawa & Inutsuka 2006;Nakatani et al 2018). To obtain the relative abundances of O , O , and O , we adopt the following procedure (see also, Fukushima et al 2020a).…”

Section: Basic Equations Of Hydrodynamicsmentioning

confidence: 99%

Radiation hydrodynamics simulations of massive star cluster formation in giant molecular clouds

Fukushima,

Yajima

2021

Preprint

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By performing three-dimensional radiation hydrodynamics simulations, we study the formation of young massive star clusters (YMCs, 𝑀 * > 10 4 𝑀 ) in clouds with the surface density ranging from Σ cl = 80 to 3200 𝑀 pc −2 . We find that photoionization feedback suppresses star formation significantly in clouds with low surface density. Once the initial surface density exceeds ∼ 100 𝑀 pc −2 for clouds with 𝑀 cl = 10 6 𝑀 and 𝑍 = 𝑍 , most of the gas is converted into stars because the photoionization feedback is inefficient in deep gravitational potential. In this case, the star clusters are massive and gravitationally bounded as YMCs. The transition surface density increases as metallicity decreases, and it is ∼ 350 𝑀 pc −2 for 𝑍 = 10 −2 𝑍 . We show that more than 10 percent of star-formation efficiency (SFE) is needed to keep a star cluster gravitationally bounded even after the disruption of a cloud. Also, we develop a semi-analytical model reproducing the SFEs obtained in our simulations. We find that the SFEs are fit with a power-law function with the dependency ∝ Σ 1/2 cl for low-surface density and rapidly increases at the transition surface densities. The conditions of the surface density and the metallicity match recent observations of giant molecular clouds forming YMCs in nearby galaxies.

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“…This atomic hydrogen column density can be translated into a hydrogen column density of 10 19−20 cm −2 depending on the stellar EUV luminosity, and therefore is used here to define the EUV heated region. Given that FUV photons can promote heating via photoelectric heating (Bakes & Tielens 1994) in the disk atmosphere, these photons are attenuated by dust once the hydrogen column density is between 10 21 and 10 22 cm −2 (Gorti et al 2009;Nakatani et al 2018a). When considering the radial optical depth of the FUV, the FUV opacity evaluated for graphite is about ∼10 4 cm 2 g −1 , which is in the wavelength regime between 0.2 and 0.09 µm (6 eV < hν < 13.6 eV).…”

Section: Frequency-integrated Cross Sectionsmentioning

confidence: 99%

Hydrodynamical simulations of protoplanetary disks including irradiation of stellar photons

Flores-Rivera

Flock

Nakatani

2020

A&A

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Context. In recent years hydrodynamical (HD) models have become important to describe the gas kinematics in protoplanetary disks, especially in combination with models of photoevaporation and/or magnetically driven winds. Our aim is to investigate how vertical shear instability (VSI) could influence the thermally driven winds on the surface of protoplanetary disks. Aims. In this first part of the project, we focus on diagnosing the conditions of the VSI at the highest numerical resolution ever recorded, and suggest at what resolution per scale height we obtain convergence. At the same time, we want to investigate the vertical extent of VSI activity. Finally, we determine the regions where extreme UV (EUV), far-UV (FUV), and X-ray photons are dominant in the disk. Methods. We perform global HD simulations using the PLUTO code. We adopt a global isothermal accretion disk setup, 2.5D (2 dimensions, 3 components) which covers a radial domain from 0.5 to 5.0 and an approximately full meridional extension. Our simulation runs cover a resolution from 12 to 203 cells per scale height. Results. We determine 50 cells per scale height to be the lower limit to resolve the VSI. For higher resolutions, ≥50 cells per scale height, we observe the convergence for the saturation level of the kinetic energy. We are also able to identify the growth of the “body” modes, with higher growth rate for higher resolution. Full energy saturation and a turbulent steady state is reached after 70 local orbits. We determine the location of the EUV heated region defined by Σr = 1019 cm−2 to be at HR ~ 9.7 and the FUV–X-ray heated boundary layer defined by Σr = 1022 cm−2 to be at HR ~ 6.2, making it necessary to introduce a hot atmosphere. For the first time we report the presence of small-scale vortices in the r − Z plane between the characteristic layers of large-scale vertical velocity motions. Such vortices could lead to dust concentration, promoting grain growth. Our results highlight the importance of combining photoevaporation processes in the future high-resolution studies of turbulence and accretion processes in disks.

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Radiation Hydrodynamics Simulations of Photoevaporation of Protoplanetary Disks by Ultraviolet Radiation: Metallicity Dependence

Cited by 65 publications

References 109 publications

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

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

Radiation hydrodynamics simulations of massive star cluster formation in giant molecular clouds

Hydrodynamical simulations of protoplanetary disks including irradiation of stellar photons

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