Flows of gas through a protoplanetary gap

Casassus, S.; Plas, G. van der; M., Sebastian Perez; Dent, W. R. F.; Fomalont, Ed; Hagelberg, J.; Hales, Antonio; Jordán, Andrés; Mawet, Dimitri; Ménard, F.; Wootten, Alwyn; Wilner, David J.; Hughes, A. Meredith; Schreiber, M. R.; Girard, J.; Ercolano, Barbara; Cánovas, H.; Román, Pablo E.; Salinas, Vachail

doi:10.1038/nature11769

Cited by 361 publications

(451 citation statements)

References 40 publications

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“…As our models assume p=3.5, an increase in the maximum dust grain size by a factor of ∼75, say, from 1 mm to 10 cm, could explain this drop in flux. This is borne out by a number of studies that have found cavities, gaps, spiral arms, and other asymmetries in Class II disks that may indicate the presence of planets (Isella et al 2010Andrews et al 2011Andrews et al , 2016Casassus et al 2013; Weidenschilling 1977). We find that our Class I disks, on average, are more massive than the Taurus Class II disks, likely due to dust grain processing hiding matter in larger bodies in the older Class II disks.…”

Section: Class I Versus Class Ii Disk Massesmentioning

confidence: 52%

Disk Masses for Embedded Class I Protostars in the Taurus Molecular Cloud

Sheehan

Eisner

2017

ApJ

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Class I protostars are thought to represent an early stage in the lifetime of protoplanetary disks, when they are still embedded in their natal envelope. Here we measure the disk masses of 10 Class I protostars in the Taurus Molecular Cloud to constrain the initial mass budget for forming planets in disks. We use radiative transfer modeling to produce synthetic protostar observations and fit the models to a multi-wavelength data set using a Markov Chain Monte Carlo fitting procedure. We fit these models simultaneously to our new Combined Array for Research in Millimeter-wave Astronomy 1.3 mm observations that are sensitive to the wide range of spatial scales that are expected from protostellar disks and envelopes so as to be able to distinguish each component, as well as broadband spectral energy distributions compiled from the literature. We find a median disk mass of  M 0.018 on average, more massive than the Taurus Class II disks, which have median disk mass of~ M 0.0025 . This decrease in disk mass can be explained if dust grains have grown by a factor of 75 in grain size, indicating that by the Class II stage, at a few Myr, a significant amount of dust grain processing has occurred. However, there is evidence that significant dust processing has occurred even during the Class I stage, so it is likely that the initial mass budget is higher than the value quoted here.

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Section: Class I Versus Class Ii Disk Massesmentioning

confidence: 52%

Disk Masses for Embedded Class I Protostars in the Taurus Molecular Cloud

Sheehan

Eisner

2017

ApJ

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“…We also followed a second method, based on non-parametric Bayesian image synthesis. We fit an image model to the observations at each spectral window, and in the visibility domain, by minimizing the weighted least-square distance, as previously performed in other multi-frequency analyses of ALMA data [20,32] . Since both approaches provided very similar trends, we adopted the Bayesian image synthesis, as it potentially allows for slightly finer angular detail, and the residual were more homogeneous (i.e.…”

Section: V883mentioning

confidence: 99%

Imaging the water snow-line during a protostellar outburst

Cieza

Casassus

Tobin

et al. 2016

Nature

Self Cite

198

246

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A snow-line is the region of a protoplanetary disk at which a major volatile, such as water or carbon monoxide, reaches its condensation temperature. Snowlines play a crucial role in disk evolution by promoting the rapid growth of icecovered grains 1−6 . Signatures of the carbon monoxide snow-line (at temperatures of around 20 kelvin) have recently been imaged with in the disks surrounding the pre-main-sequence stars TW Hydra 7−9 and HD163296 [3,10] , at distances of about 30 astronomical units (au) from the star. But the water snow-line of a protoplanetary disk (at temperatures of more than 100 kelvin) has not hitherto been seen, as it generally lies very close to the star (less than 5 au away for solartype stars 11 ). Water-ice is important because it regulates the efficiency of dust and planetesimal coagulation 5 , and the formation of comets, ice giants and the cores of gas giants 12 . Here we report ALMA images at 0.03-arcsec resolution (12 au) of the protoplanetary disk around V883 Ori, a protostar of 1.3 solar masses that is undergoing an outburst in luminosity arising from a temporary increase in the accretion rate 13 . We find an intensity break corresponding to an abrupt change in the optical depth at about 42 au, where the elevated disk temperature approaches the condensation point of water, from which we conclude that the outburst has moved the water snow-line. The spectral behaviour across the snow-line confirms recent model predictions 14 : dust fragmentation and the inhibition of grain growth at higher temperatures results in soaring grain number densities and optical depths. As most planetary systems are expected to experience outbursts caused by accretion during their formation [15,16] our results imply that highly dynamical water snow-lines must be considered when developing models of disk evolution and planet formation. V883Ori is an FU Ori object identified as such by [17] from followup spectroscopy of deeply embedded sources from the Infrared Astronomical Satellite (IRAS). It is located in the Orion Nebula Cluster, which has a distance of 414±7 pc [18] . It has a disk mass of 0.3 M and a bolometric luminosity of 400 L [19] . We have obtained 230 GHz/1.3 mm (band-6) observations of V883 Ori using the Atacama Large Millimeter/submillimeter Array (ALMA) in four different array configurations with baselines ranging from 14 m to 12.6 km, which were taken in ALMA Cycle-2 and Cycle-3. These new ALMA observations include continuum and the 12 CO, 13 CO, and C 18 O J = 2 -1 spectral lines. We use the C 18 O gas line to investigate the dynamics of the system at 0.2 (90 au) resolution and the continuum data to constrain the physical properties of the dust in the V883 Ori disk at 0.03 (12 au) resolution. In Figure 1 (top panel) we show our Cycle-3 continuum image at 0.03 resolution, the highest resolution ever obtained for a FU Ori object at millimeter wavelengths. We find that the V883 Ori disk has a two-region morphology, with a very bright inner disk (r ∼ 0.1 , 42 au) and a much more tenuous outer dis...

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“…As the inner discs are depleted by accretion onto the stars on timescales of few 10 3 yr, replenishing material must be transferred from the outer reservoir in order to fuel 1 planet formation (which occurs on timescales of ∼1 Myr). Gas flowing through disc cavities has been detected in single star systems 6 . A circumbinary disc was discovered around the young low-mass binary system GGTau-A 7 , which has recently been proven to be a hierarchical triple system 8 .…”

mentioning

confidence: 99%

Possible planet formation in the young, low-mass, multiple stellar system GG Tau A

Dutrey

Folco

Guilloteau

et al. 2014

Nature

105

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Forming planets around binary stars may be more difficult than around single stars [1][2][3] . In a close binary star (< 100 au separation), theory predicts the presence of circumstellar discs around each star, and an outer circumbinary disc surrounding a gravitationally cleared inner cavity 4,5 . As the inner discs are depleted by accretion onto the stars on timescales of few 10 3 yr, replenishing material must be transferred from the outer reservoir in order to fuel 1 planet formation (which occurs on timescales of ∼1 Myr). Gas flowing through disc cavities has been detected in single star systems 6 . A circumbinary disc was discovered around the young low-mass binary system GGTau-A 7 , which has recently been proven to be a hierarchical triple system 8 . It has one large inner disc 9 around the southern single star and shows small amounts of shocked H 2 gas residing within the central cavity 10 , but other than a weak detection 11 , hitherto the distribution of cold gas in this cavity or in any other binary or multiple star system has never been determined. Here we report imaging of massive CO-emitting gas fragments within the GG Tau-A cavity. From the kinematics we conclude that the flow appears capable of sustaining the inner disc beyond the accretion lifetime, leaving time for planet formation to occur.The 1-5 Million year old 12, 13 triple stellar system GGTau-A is located at 140 pc in a hole of the Taurus molecular cloud. Its molecular emission is free of contamination 14 and there is no known outflow neither jet associated to the source. The main binary GGTau-A (Aa-Ab) and the close-binary GGTau-Ab (Ab1-Ab2) have an apparent separation of 35 au and 4.5 au, respectively 8 .The outer circumbinary Keplerian disc of gas and dust surrounding GGTau-A consists of a ring extending from radius r ∼ 190 to 280 au and an outer disc extending up to 800 au from the central stars with a total mass ∼ 0.15 M ⊙ 14 .Using the Atacama Large Millimetre Array (ALMA), we observed GGTau-A in the dust thermal emission at 0.45 mm and in CO J=6-5 line ( Fig.1: panels a,b,c) with an angular resolution θ ≃ 0.25 ′′ or ∼35 au. The continuum image shows cold dust emission from only one circumstellar 2 disc-like structure associated with GGTau-Aa 9, 15 . We estimate the minimum dust disc size to be ∼ 7 au while the minimum mass of gas and dust is roughly 10 −3 M ⊙ about Jupiter's mass. The complex CO J=6-5 spectral line shape at the location of GGTau-Aa also reveals the existence of a CO circumstellar disc of outer radius ∼ 20 au (Methods and Extended Data: Fig.2). We do not detect cold dust emission around GGTau-Ab even though the existence of inner dust disc(s) was reported from unresolved Infrared emission 16 . Our 0.45 mm upper limits (Methods) are compatible with tidal truncation which prevents any circumstellar disc to extend beyond about 2 au 8 .The ALMA CO J=6-5 image ( Fig.1 panels a,b,c and Extended Data: Fig.1 and Fig.2) also clearly resolves CO gas within the central cavity with a structure indicative of the streamer-like f...

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Flows of gas through a protoplanetary gap

Cited by 361 publications

References 40 publications

Disk Masses for Embedded Class I Protostars in the Taurus Molecular Cloud

Disk Masses for Embedded Class I Protostars in the Taurus Molecular Cloud

Imaging the water snow-line during a protostellar outburst

Possible planet formation in the young, low-mass, multiple stellar system GG Tau A

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