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

Wölfer, Lisa; Picogna, Giovanni; Ercolano, Barbara; Dishoeck, E. F. van

doi:10.1093/mnras/stz2939

Cited by 38 publications

(36 citation statements)

References 36 publications

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“…Recent works from , Ercolano et al (2018), andWölfer et al (2019) suggest that photoevaporation is more effective in disks that are depleted from carbon and oxygen, which results in higher mass-loss rates and a faster dispersal of the outer disk. The outcome of this approach is a lower fraction of relics (up to 45%), which is much lower than standard photoevaporative models, and better suited to explain observations.…”

Section: Comparison With the Observed Transition Disk Populationmentioning

confidence: 99%

“…Additional improvements for the model would be to include stars of different masses, considering their respective photoevaporation mass-loss rates (Komaki et al 2021), the evolution of the stellar luminosity during the first million years after formation (Kunitomo et al 2021), and the effect of carbon depletion, which leads to stronger photoevaporation rates (Ercolano et al 2018;Wölfer et al 2019).…”

Section: Comparison With the Observed Transition Disk Populationmentioning

confidence: 99%

“…Though photoevaporation models can easily predict large gaps that extend for tens of AU, these fail to explain the observed high accretion rates, since the gaseous inner disks are short lived and quickly accreted once the gap opens (Owen et al 2010(Owen et al , 2011Picogna et al 2019). As a consequence, these models tend to over-predict the fraction of non-accreting disks with gaps that extend beyond 20 AU, although the mechanisms that speed up the depletion of the outer disk, such as thermal sweeping and depletion of carbon and oxygen, can partially alleviate the discrepancy with observations (Owen et al 2013;Ercolano et al 2018;Wölfer et al 2019).…”

Section: Introductionmentioning

confidence: 99%

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

Gárate

Delage

Stadler

et al. 2021

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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: Comparison With the Observed Transition Disk Populationmentioning

confidence: 99%

Section: Comparison With the Observed Transition Disk Populationmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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

Gárate

Delage

Stadler

et al. 2021

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“…For the gas-loss rate due to photoevaporation, we followed Picogna et al (2019) (X-ray and extreme UV). Carbon depletion can have significant effects (Wölfer et al 2019) that we did not take into account. For the profile provided by Picogna et al (2019) we used the scaling with stellar mass from Owen et al (2012).…”

Section: Appendix A: Photoevaporationmentioning

confidence: 99%

Constraining the parameter space for the solar nebula

Lenz

Klahr

Birnstiel

et al. 2020

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Context. When we wish to understand planetesimal formation, the only data set we have is our own Solar System. The Solar System is particularly interesting because so far, it is the only planetary system we know of that developed life. Understanding the conditions under which the solar nebula evolved is crucial in order to understand the different processes in the disk and the subsequent dynamical interaction between (proto-)planets after the gas disk has dissolved. Aims. Protoplanetary disks provide a plethora of different parameters to explore. The question is whether this parameter space can be constrained, allowing simulations to reproduce the Solar System. Methods. Models and observations of planet formation provide constraints on the initial planetesimal mass in certain regions of the solar nebula. By making use of pebble flux-regulated planetesimal formation, we performed a parameter study with nine different disk parameters such as the initial disk mass, the initial disk size, the initial dust-to-gas ratio, the turbulence level, and others. Results. We find that the distribution of mass in planetesimals in the disk depends on the timescales of planetesimal formation and pebble drift. Multiple disk parameters can affect the pebble properties and thus planetesimal formation. However, it is still possible to draw some conclusions on potential parameter ranges. Conclusions. Pebble flux-regulated planetesimal formation appears to be very robust, allowing simulations with a wide range of parameters to meet the initial planetesimal constraints for the solar nebula. This means that it does not require much fine-tuning.

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“…In the first paper of this series (Picogna et al 2019, hereafter Paper I) we showed the dependence between the stellar X-ray luminosity and the mass-loss rate due to thermal winds generated by the XEUV heating from the central star. Then we studied the influence of carbon depletion (Wölfer et al 2019) and stellar spectra hardness on the mass-loss rates (Ercolano et al 2021, hereafter Paper II). In this following work, we focus on stellar mass dependence and how it might influence disc evolution.…”

Section: Introductionmentioning

confidence: 99%

The dispersal of protoplanetary discs -- III: Influence of stellar mass on disc photoevaporation

Picogna,

Ercolano,

Espaillat

2021

Preprint

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The strong X-ray irradiation from young solar-type stars may play a crucial role in the thermodynamics and chemistry of circumstellar discs, driving their evolution in the last stages of disc dispersal as well as shaping the atmospheres of newborn planets. In this paper we study the influence of stellar mass on circumstellar disc mass-loss rates due to X-ray irradiation, extending our previous study of the mass-loss rate's dependence on the X-ray luminosity and spectrum hardness. We focus on stars with masses between 0.1 and 1 M , which are the main target of current and future missions to find potentially habitable planets. We find a linear relationship between the mass-loss rates and the stellar masses when changing the X-ray luminosity accordingly with the stellar mass. This linear increase is observed also when the X-ray luminosity is kept fixed because of the lower disc aspect ratio which allows the X-ray irradiation to reach larger radii. We provide new analytical relations for the massloss rates and profiles of photoevaporative winds as a function of the stellar mass that can be used in disc and planet population synthesis models. Our photoevaporative models correctly predict the observed trend of inner-disc lifetime as a function of stellar mass with an increased steepness for stars smaller than 0.3 M , indicating that X-ray photoevaporation is a good candidate to explain the observed disc dispersal process.

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

Cited by 38 publications

References 36 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

Constraining the parameter space for the solar nebula

The dispersal of protoplanetary discs -- III: Influence of stellar mass on disc photoevaporation

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