On the maximum grain size entrained by photoevaporative winds

Hutchison, Mark; Laibe, Guillaume; Maddison, Sarah

doi:10.1093/mnras/stw2191

Cited by 44 publications

(39 citation statements)

References 36 publications

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“…Our model is intended to be combined with a vertical mixing prescription later on in order to extract a realistic dust density distribution in the wind. So we may very well, just as Hutchison et al (2016a) note they did, model grain sizes that will not migrate far enough vertically to actually Article number, page 3 of 18 A&A proofs: manuscript no. Draft Fig.…”

Section: Initial Positioningmentioning

confidence: 99%

“…7 for M * = 0.75 M ) (orange, peak at around 40 AU), we can see the size enhancement -especially at smaller R -caused by the inclusion of X-rays in our photoevaporative wind model. The blue dashed line represents our results scaled down by a factor of 3, to compensate for the differing internal grain densities of Hutchison et al (2016a) and this work; yet,Ṁw still differs between the models, making a direct comparison difficult. The MHD wind model investigated by Miyake et al (2016, their Fig.…”

Section: Maximum Entrained Grain Sizementioning

confidence: 99%

“…Previous investigations of dust entrainment in photoevaporative winds have limited themselves to EUV-only photoevaporation (Owen et al 2011a;Hutchison et al 2016a). Fig.…”

Section: Comparison To Euv Wind Modelsmentioning

confidence: 99%

“…radius) can be lifted up and blown out by an EUV-driven wind around a Herbig Ae/Be star. More recently, Hutchison et al (2016a) have investigated EUV-driven dust outflow by means of a two-fluid smoothed particle hydrodynamics (SPH) code (Hutchison et al 2016b); they find entrainment of grains of up to 4 µm around a 0.75 M T-Tauri star (although they note that this value may drop to about 1 µm due to grains settling towards the disk midplane). Both Owen et al (2011a) and Hutchison et al (2016a) show that the wind selectively en-Article number, page 1 of 18 arXiv:2001.10545v1 [astro-ph.EP] 28 Jan 2020 A&A proofs: manuscript no.…”

Section: Introductionmentioning

confidence: 99%

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Dust entrainment in photoevaporative winds: The impact of X-rays

Franz

Picogna

Ercolano

et al. 2020

A&A

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Context. X-ray-and EUV-(XEUV-) driven photoevaporative winds acting on protoplanetary disks around young T-Tauri stars may crucially impact disk evolution, affecting both gas and dust distributions. Aims. We investigate the dust entrainment in XEUV-driven photoevaporative winds and compare our results to existing MHD and EUV-only models. Methods. We used a 2D hydrodynamical gas model of a protoplanetary disk irradiated by both X-ray and EUV spectra from a central T-Tauri star to trace the motion of passive Lagrangian dust grains of various sizes. The trajectories were modelled starting at the disk surface in order to investigate dust entrainment in the wind. Results. For an X-ray luminosity of LX = 2·10 30 erg/s emitted by a M * = 0.7 M star, corresponding to a wind mass-loss rate ofṀw 2.6 · 10 −8 M /yr, we find dust entrainment for sizes a0 11 µm (9 µm) from the inner 25 AU (120 AU). This is an enhancement over dust entrainment in less vigorous EUV-driven winds withṀw 10 −10 M /yr. Our numerical model also shows deviations of dust grain trajectories from the gas streamlines even for µm-sized particles. In addition, we find a correlation between the size of the entrained grains and the maximum height they reach in the outflow.Conclusions. X-ray-driven photoevaporative winds are expected to be dust-rich if small grains are present in the disk atmosphere.Key words. protoplanetary disks -stars: T-Tauri -dust entrainment -photoevaporative winds: XEUV -methods: numerical -silicate grains -young stellar objects -interstellar dust processes 1 The ionization parameter is defined as ξ = L * /(n r 2 ), with L * the stellar luminosity, n the gas density, and r the (spherical) radial distance from the star. 2 '2.5D' meaning a 2D coordinate system (r, ϑ) with 3D velocity information (vr, v ϑ , vϕ).Article number, page 2 of 18 R. Franz et al.: Dust entrainment in photoevaporative winds: The impact of X-rays

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Section: Initial Positioningmentioning

confidence: 99%

Section: Maximum Entrained Grain Sizementioning

confidence: 99%

“…Previous investigations of dust entrainment in photoevaporative winds have limited themselves to EUV-only photoevaporation (Owen et al 2011a;Hutchison et al 2016a). Fig.…”

Section: Comparison To Euv Wind Modelsmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Dust entrainment in photoevaporative winds: The impact of X-rays

Franz

Picogna

Ercolano

et al. 2020

A&A

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“…The variable P Cygni profile of the He I line is likely related to a wind whose orientation changes on timescales of a day or less (Sitko et al 2012) which is launched in the star-disk interaction region (e.g., Edwards 2009). Micron-sized dust grains in the inner disk atmosphere could be entrained by a photoevaporative wind that is driven by the UV radiation of the star (Owen et al 2011;Hutchison et al 2016) or dust could be uplifted by a centrifugally driven disk wind (Bans & Königl 2012). An extended low-density atmosphere could be supported by the magnetic field of the inner disk which may explain a large near-infrared excess and possible shadowing (Turner et al 2014).…”

Section: Inner Disk Processes Affecting the Dust Dynamicsmentioning

confidence: 99%

Variable Dynamics in the Inner Disk of HD 135344B Revealed with Multi-epoch Scattered Light Imaging^∗

Stolker

Sitko

Lazareff

et al. 2017

ApJ

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We present multi-epoch Very Large Telescope/Spectro-Polarimetric High-contrast Exoplanet REsearch observations of the protoplanetary disk around HD 135344B (SAO 206462). The J-band scattered light imagery reveal, with high spatial resolution (∼41 mas, 6.4 au), the disk surface beyond ∼20 au. Temporal variations are identified in the azimuthal brightness distributions of all epochs, presumably related to the asymmetrically shading dust distribution in the inner disk. These shadows manifest themselves as narrow lanes, cast by localized density enhancements, and broader features which possibly trace the larger scale dynamics of the inner disk. We acquired visible and near-infrared photometry which shows variations up to 10% in the JHK bands, possibly correlated with the presence of the shadows. Analysis of archival Very Large Telescope Interferometer/PIONIER H-band visibilities constrain the orientation of the inner disk to i = 18.• 2 +3.4−4.1 and PA = 57.• 3 ± 5.• 7, consistent with an alignment with the outer disk or a minor disk warp of several degrees. The latter scenario could explain the broad, quasi-stationary shadowing in N-NW direction in case the inclination of the outer disk is slightly larger. The correlation between the shadowing and the near-infrared excess is quantified with a grid of radiative transfer models. The variability of the scattered light contrast requires extended variations in the inner disk atmosphere (H/r 0.2). Possible mechanisms that may cause asymmetric variations in the optical depth (∆τ 1) through the atmosphere of the inner disk include turbulent fluctuations, planetesimal collisions, or a dusty disk wind, possibly enhanced by a minor disk warp. A fine temporal sampling is required to follow day-to-day changes of the shadow patterns which may be a face-on variant of the UX Orionis phenomenon.

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