Dust delivery and entrainment in photoevaporative winds

Hutchison, Mark; Clarke, C. J.

doi:10.1093/mnras/staa3608

Cited by 25 publications

(28 citation statements)

References 77 publications

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“…where Σ d is the dust surface density (of a particular dust species), and Σw,d is the dust-loss rate due to entrainment with the photoevaporative wind (Hutchison et al 2016;Franz et al 2020;Hutchison & Clarke 2021;Booth & Clarke 2021), which we describe below. In this work, we ignored the effects of the dust back-reaction onto the gas dynamics, since these become negligible at low dust-to-gas ratios ( ≤ 0.01) and over timescales longer than 1 Myr (Gárate et al 2020).…”

Section: Dust Evolutionmentioning

confidence: 99%

Large gaps and high accretion rates in photoevaporative transition disks with a dead zone

Gárate

Delage

Stadler

et al. 2021

A&A

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Context. Observations of young stars hosting transition disks show that several of them have high accretion rates, despite their disks presenting extended cavities in their dust component. This represents a challenge for theoretical models, which struggle to reproduce both features simultaneously. Aims. We aim to explore if a disk evolution model, including a dead zone and disk dispersal by X-ray photoevaporation, can explain the high accretion rates and large gaps (or cavities) measured in transition disks. Methods. We implemented a dead zone turbulence profile and a photoevaporative mass-loss profile into numerical simulations of gas and dust. We performed a population synthesis study of the gas component and obtained synthetic images and SEDs of the dust component through radiative transfer calculations. Results. This model results in long-lived inner disks and fast dispersing outer disks that can reproduce both the accretion rates and gap sizes observed in transition disks. For a dead zone of turbulence αdz = 10−4 and an extent rdz = 10 AU, our population synthesis study shows that 63% of our transition disks are still accreting with Ṁg ≥ 10−11 M⊙ yr−1 after opening a gap. Among those accreting transition disks, half display accretion rates higher than 5.0 × 10−10 M⊙ yr−1. The dust component in these disks is distributed in two regions: in a compact inner disk inside the dead zone, and in a ring at the outer edge of the photoevaporative gap, which can be located between 20 and 100 AU. Our radiative transfer calculations show that the disk displays an inner disk and an outer ring in the millimeter continuum, a feature that resembles some of the observed transition disks. Conclusions. A disk model considering X-ray photoevaporative dispersal in combination with dead zones can explain several of the observed properties in transition disks, including the high accretion rates, the large gaps, and a long-lived inner disk at millimeter emission.

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Section: Dust Evolutionmentioning

confidence: 99%

Large gaps and high accretion rates in photoevaporative transition disks with a dead zone

Gárate

Delage

Stadler

et al. 2021

A&A

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“…Admittedly, our dust removal prescription is idealized in many aspects and therefore bears some uncertainties. We first note that our prescription differs with those photoevaporative disc wind models applicable to the outer regions of PPDs (Hutchison & Clarke 2021;. The driving mechanism for funnel flows is the magneto-centrifugal force that dominates the pressure gradient in the low-density disc atmosphere above ∼ 𝐻 (Blandford & Payne 1982;Wardle & Koenigl 1993).…”

Section: Limitationsmentioning

confidence: 94%

Dust Accumulation near the Magnetospheric Truncation of Protoplanetary Discs around T Tauri Stars

Li,

Chen,

Lin

2021

Preprint

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The prevalence of short-period super-Earths that are independent of host metallicity challenges the theoretical construction of their origin. We propose that dust trapping in the global pressure bump induced by magnetospheric truncation in evolved protoplanetary discs (PPDs) around T Tauri stars offers a promising formation mechanism for super-Earths, where the host metallicity is already established. To better understand this planet forming scenario, we construct a toy inner disc model and focus on the evolution of dust trapped in the bump, taking into account the supply from drifting pebbles and loss due to funnel flows. We develop an implicit coagulation-fragmentation code, Rubble, and perform a suite of simulations to evolve the local dust size distributions. Our study for the first time considers dust feedback effect on turbulent diffusion in this kind of model. We report that efficient dust growth and significant accumulation of dust mass is possible in less turbulent disc with sturdier solids and with faster external supply, laying out a solid foundation for further growth towards planetesimals and planetary embryos. We further find that, depending on the dominant process, solid mass may predominantly accumulate in cm-sized grains or particles in runaway growth, indicating different ways of forming planetesimals. Furthermore, these various outcomes show different efficiencies in saving dust from funnel flows, suggesting that they may be distinguishable by constraining the opacity of funnel flows. Also, these diverse dust behaviours may help explain the observed dipper stars and rapidly varying shadows in PPDs.

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“…Their (almost) vertical launch into the wind even from there, and for all grain sizes, corroborates the assumption of a vertical launch from a non-angled surface made by Clarke & Alexander (2016) for a semi-analytical EUV-only gas model. These have since been refined to include dust by Hutchison & Clarke (2021), and extended to allow for various launching angles by Sellek et al (2021). The qualitative agreement between our numerical results and the semi-analytical work above would suggest that in theory costly hydrodynamical simulations as presented in this work could be replaced by semi-analytical formulations.…”

Section: Trajectoriesmentioning

confidence: 99%

“…The presence of disk winds can be inferred in a variety of ways; for instance, Monsch et al (2019Monsch et al ( , 2021a predicted orbital distributions of hot Jupiters in XEUVirradiated disks, and , Ercolano & Owen (2016), and Weber et al (2020) modelled line profiles for disks impacted by photoevaporation. Furthermore, Owen et al (2011), Hutchison et al (2016a,b), , and Hutchison & Clarke (2021) have worked to model and analytically formulate dust entrainment in photoevaporative winds. In Franz et al (2020, henceforth Paper I) and Franz et al (2022, henceforth Paper II), we numerically simulated the dust content and observability of dusty XEUV-driven outflows around a primordial protoplanetary disk based on the hydrodynamical (HD) models of Picogna et al (2019) (which have since been refined by Ercolano et al 2021;Picogna et al 2021).…”

Section: Introductionmentioning

confidence: 99%

Dust entrainment in photoevaporative winds: Synthetic observations of transition disks

Franz,

Picogna,

Ercolano

et al. 2022

Preprint

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Context. X-ray-and extreme-ultraviolet-(XEUV-) driven photoevaporative winds acting on protoplanetary disks around young T-Tauri stars may strongly impact disk evolution, affecting both gas and dust distributions. Small dust grains in the disk are entrained in the outflow and may produce a detectable signal. In this work, we investigate the possibility of detecting dusty outflows from transition disks with an inner cavity. Aims. We compute dust densities for the wind regions of XEUV-irradiated transition disks and determine whether they can be observed at wavelengths 0.7 λ obs [µm] 1.8 with current instrumentation. Methods. We simulated dust trajectories on top of 2D hydrodynamical gas models of two transition disks with inner holes of 20 and 30 AU, irradiated by both X-ray and EUV spectra from a central T-Tauri star. The trajectories and two different settling prescriptions for the dust distribution in the underlying disk were used to calculate wind density maps for individual grain sizes. Finally, the resulting dust densities were converted to synthetic observations in scattered and polarised light. Results. For an XEUV-driven outflow around a M * = 0.7 M T-Tauri star with LX = 2 • 10 30 erg/s, we find dust massloss rates Ṁdust 2.0 • 10 −3 Ṁgas, and if we invoke vertical settling, the outflow is quite collimated. The synthesised images exhibit a distinct chimney-like structure. The relative intensity of the chimneys is low, but their detection may still be feasible with current instrumentation under optimal conditions. Conclusions. Our results motivate observational campaigns aimed at the detection of dusty photoevaporative winds in transition disks using JWST NIRCam and SPHERE IRDIS.

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Dust delivery and entrainment in photoevaporative winds

Cited by 25 publications

References 77 publications

Large gaps and high accretion rates in photoevaporative transition disks with a dead zone

Large gaps and high accretion rates in photoevaporative transition disks with a dead zone

Dust Accumulation near the Magnetospheric Truncation of Protoplanetary Discs around T Tauri Stars

Dust entrainment in photoevaporative winds: Synthetic observations of transition disks

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