Hydrocarbon Emission Rings in Protoplanetary Disks Induced by Dust Evolution

Bergin, Edwin A.; Du, Fujun; Cleeves, L. Ilsedore; Blake, Geoffrey A.; Schwarz, Kamber R.; Visser, R.; Zhang, Ke

doi:10.3847/0004-637x/831/1/101

Cited by 215 publications

(330 citation statements)

References 104 publications

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“…Using models that include detailed modeling of the CO and H 2 O chemistry, studies found that the disk surrounding TW Hya is genuinely depleted in volatile carbon and oxygen (e.g., Bergin et al 2010;Bergin et al 2013;Hogerheijde et al 2011;Favre et al 2013;Du et al 2015). Recent observations of [CI], [CII], [OI], C 2 H and C 3 H 2 have reinforced this conclusion (Kama et al 2016b;Bergin et al 2016). …”

Section: Case Study: Tw Hyamentioning

confidence: 68%

“…Of particular interest is the protoplanetary disk of TW Hya (59.54 ± 1.45 pc, Astraatmadja & Bailer-Jones 2016), where the gas mass estimated using HD is more than one order of magnitude higher than the gas mass estimated using C 18 O (Favre et al 2013). Different studies have shown that the TW Hya disk seems genuinely depleted in volatile carbon and oxygen (e.g., Bergin et al 2010;Bergin et al 2013Bergin et al , 2016Hogerheijde et al 2011;Favre et al 2013;Du et al 2015;Kama et al 2016b). Recently, new observations of the CO isotopologues have become available (see, e.g., Schwarz et al 2016).…”

Section: Introductionmentioning

confidence: 99%

“…A possible explanation could be grain growth, where carbon has been locked up in large icy bodies that no longer participate in the gas-phase chemistry (see, e.g., Bergin et al 2010;Bergin et al 2016;Du et al 2015;Kama et al 2016b). Another cause could be the conversion of CO into more complex species.…”

Section: Introductionmentioning

confidence: 99%

“…However, studies that include these effects find that overall gas phase carbon must still be additionally depleted by a factor 10- 100. This leads to low CO emission even for massive disks (e.g., Bruderer et al 2012;Favre et al 2013;Du et al 2015;Kama et al 2016b;Bergin et al 2016).…”

Section: Introductionmentioning

confidence: 99%

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Far-infrared HD emission as a measure of protoplanetary disk mass

Trapman

Miotello

Kama

et al. 2017

A&A

101

138

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Context. Protoplanetary disks around young stars are the sites of planet formation. While the dust mass can be estimated using standard methods, determining the gas mass -and thus the amount of material available to form giant planets -has proven to be very difficult. Hydrogen deuteride (HD) is a promising alternative to the commonly-used gas mass tracer, carbon monoxide. However, its potential has not yet been investigated with models incorporating both HD and CO isotopologue-specific chemistry, and its sensitivity to uncertainties in disk parameters has not yet been quantified. Aims. To examine the robustness of HD as tracer of the disk gas mass, specifically the effect of gas mass on the HD far infrared emission and its sensitivity to the vertical structure. Also, to provide requirements for future far-infrared missions such as SPICA. Methods. Deuterium chemistry reactions relevant for HD were implemented in the thermochemical code DALI and more than 160 disk models were run for a range of disk masses and vertical structures. Results. The HD J=1-0 line intensity depends directly on the gas mass through a sublinear power law relation with a slope of ∼0.8. Assuming no prior knowledge about the vertical structure of a disk and using only the HD 1-0 flux, gas masses can be estimated to within a factor of two for low mass disks (M disk ≤ 10 −3 M ). For more massive disks, this uncertainty increases to more than an order of magnitude. Adding the HD 2-1 line or independent information about the vertical structure can reduce this uncertainty to a factor of ∼ 3 for all disk masses. For TW Hya, using the radial and vertical structure from Kama et al. (2016b) the observations constrain the gas mass to 6 · 10 −3 M ≤ M disk ≤ 9 · 10 −3 M . Future observations require a 5σ sensitivity of 1.8 · 10 −20 W m −2 (2.5 · 10 −20 W m −2 ) and a spectral resolving power R ≥ 300 (1000) to detect HD 1-0 (HD 2-1) for all disk masses above 10 −5 M with a line-to-continuum ratio ≥ 0.01. Conclusions. These results show that HD can be used as an independent gas mass tracer with a relatively low uncertainty and should be considered as an important science goal for future far-infrared missions.

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Section: Case Study: Tw Hyamentioning

confidence: 68%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

See 2 more Smart Citations

Far-infrared HD emission as a measure of protoplanetary disk mass

Trapman

Miotello

Kama

et al. 2017

A&A

101

138

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“…The disk displays a variety of substructures and radial morphologies in scattered light (Debes et al 2013;Akiyama et al 2015;Rapson et al 2015;van Boekel et al in press. ), mmdust continuum (Andrews et al 2012;Menu et al 2014;Andrews et al 2016;Tsukagoshi et al 2016) and molecular line emission (Qi et al 2013;Kastner et al 2015;Nomura et al 2016;Schwarz et al 2016;Bergin et al 2016), with many physical and chemical processes being invoked to explain these striking features.…”

Section: Introductionmentioning

confidence: 99%

A Surface Density Perturbation in the TW Hydrae Disk at 95 au Traced by Molecular Emission

Teague

Semenov

Gorti

et al. 2017

ApJ

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We present ALMA Cycle 2 observations at 0.5 resolution of TW Hya of CS J = 5 − 4 emission. The radial profile of the integrated line emission displays oscillatory features outwards of 1.5 (≈ 90 au). A dip-like feature at 1.6 is coincident in location, depth and width with features observed in dust scattered light at near-infrared wavelengths. Using a thermochemical model indicative of TW Hya, gas-grain chemical modelling and non-LTE radiative transfer, we demonstrate that such a feature can be reproduced with a surface density depression, consistent with the modelling performed for scattered light observations of TW Hya. We further demonstrate that a gap in the dust distribution and dust opacity only cannot reproduce the observed CS feature. The outer enhancement at 3.1 is identified as a region of intensified desorption due to enhanced penetration of the interstellar FUV radiation at the exponential edge of the disk surface density, which intensifies the photochemical processing of gas and ices.

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Chemistry During the Gas-Rich Stage of Planet Formation

Bergin¹,

Cleeves²

2018

Handbook of Exoplanets

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In this chapter we outline some of the basic understanding of the chemistry that accompanies planet formation. We discuss the basic physical environment which dictates the dominant chemical kinetic pathways for molecule formation. We focus on three zones from both observational and theoretical perspectives: (1) the planet forming midplane and ice/vapor transition zones (snow-lines), (2) the warm disk surface that is shielded from radiation, which can be readily accessed by todays observational facilities, and (3) the surface photodissociation layers where stellar radiation dominates. We end with a discussion of how chemistry influences planet formation along with how to probe the link between formation and ultimate atmospheric composition for gas giants and terrestrial worlds.

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Hydrocarbon Emission Rings in Protoplanetary Disks Induced by Dust Evolution

Cited by 215 publications

References 104 publications

Far-infrared HD emission as a measure of protoplanetary disk mass

Far-infrared HD emission as a measure of protoplanetary disk mass

A Surface Density Perturbation in the TW Hydrae Disk at 95 au Traced by Molecular Emission

Chemistry During the Gas-Rich Stage of Planet Formation

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