Compact Disks in a High-resolution ALMA Survey of Dust Structures in the Taurus Molecular Cloud

Long, Feng; Herczeg, Gregory J.; Harsono, Daniel; Pinilla, P.; Tazzari, Marco; Manara, C. F.; Pascucci, Ilaria; Cabrit, S.; Nisini, B.; Johnstone, Doug; Edwards, Suzan; Salyk, Colette; Ménard, F.; Lodato, Giuseppe; Boehler, Yann; Mace, Gregory N.; Liu, Yao; Mulders, Gijs D.; Hendler, Nathanial P.; Ragusa, Enrico; Fischer, William J.; Banzatti, Andrea; Rigliaco, E.; Plas, Gerrit van de; Dipierro, Giovanni; Gully-Santiago, Michael; López-Valdivia, Ricardo

doi:10.3847/1538-4357/ab2d2d

Cited by 226 publications

(358 citation statements)

References 116 publications

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“…Figure 2 present these HST data from which we could measure the position angle of the optical jet. The main focus of this paper is on the study of the large scale molecular gas emission near DO Tauri, but we also report the characteristics of the disk dust emission, spatially resolved here, and its associated CO (2-1) emission (see also the recently reported ALMA results by Long et al 2019, analogous to these simultaneously derived here). The disk is detected at 1.3 mm continuum ( Figure 1) with an intensity peak of 24.55±0.06 mJy beam −1 and a flux density of 116.8±0.1 mJy, consistent with the 125.4±3.5 mJy reported by Kwon et al (2015) at a similar frequency.…”

Section: Hst Archive Observationsmentioning

confidence: 70%

“…Note that this is roughly a circular disk, with a 47 au radius and the uncertainty of its position angle and inclination may be larger than that provided by the statistical procedure. Therefore, we estimate the uncertainty of the disk PA and inclination as the difference with the same quantities derived by Long et al (2019). For a circular disk, this fit implies an inclination of 19 • ±9 • with respect to the plane of the sky.…”

Section: Hst Archive Observationsmentioning

confidence: 97%

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A Ringed Pole-on Outflow from DO Tauri Revealed by ALMA

Fernández-López¹,

Zapata²,

Rodrı́guez³

et al. 2020

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We present new ALMA Band 6 observations including the CO (2-1) line and 1.3 mm continuum emission from the surroundings of the young stellar object DO Tauri. The ALMA CO molecular data show three different series of rings at different radial velocities. These rings have radii around 220 au and 800 au. We make individual fits to the rings and note that their centers are aligned with DO Tauri and its optical highvelocity jet. In addition, we notice that the velocity of these structures increases with the separation from the young star. We discuss the data under the hypothesis that the rings represent velocity cuts through three outflowing shells that are possibly driven by a wide-angle wind, dragging the environment material along a direction close to the line of sight (i= 19 • ). We estimate the dynamical ages, the mass, the momentum and the energy of each individual outflow shell and those of the whole outflow. The results are in agreement with those found in outflows from Class II sources. We make a rough estimate for the size of the jet/wind launching region, which needs to be of 15 au. We report the physical characteristics of DO Tauri's disk continuum emission (almost face-on and with a projected major axis in the north-south direction) and its velocity gradient orientation (north-south), indicative of disk rotation for a 1-2 M central star. Finally we show an HST [SII] image of the optical jet and report a measurement of its orientation in the plane of the sky.

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Section: Hst Archive Observationsmentioning

confidence: 70%

Section: Hst Archive Observationsmentioning

confidence: 97%

A Ringed Pole-on Outflow from DO Tauri Revealed by ALMA

Fernández-López¹,

Zapata²,

Rodrı́guez³

et al. 2020

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show abstract

“…These observed disks surrounding a range of host-stellar masses have gas radii in the range of 63-500 AU at an age of ∼ 1-3 Myr. We emphasize, however, that these large, extended disks are the exception and are not indicative of typical disks that are much more compact, as indicated by numerous observations showing dust radii of 20 − 30 AU (Barenfeld et al 2016(Barenfeld et al , 2017Cox et al 2017;Hendler et al 2017;Tazzari et al 2017;Cieza et al 2019;Long et al 2019).…”

Section: Introductionmentioning

confidence: 66%

Formation of planetary populations − II. Effects of initial disc size and radial dust drift

Alessi

Cridland

2020

Monthly Notices of the Royal Astronomical Society

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Recent ALMA observations indicate that while a range of disk sizes exist, typical disk radii are small, and that radial dust drift affects the distribution of solids in disks.Here we explore the consequences of these features in planet population synthesis models. A key feature of our model is planet traps -barriers to otherwise rapid type-I migration of forming planets -for which we include the ice line, heat transition, and outer edge of the dead zone. We find that the ice line plays a fundamental role in the formation of warm Jupiters. In particular, the ratio of super Earths to warm Jupiters formed at the ice line depend sensitively on the initial disk radius. Initial gas disk radii of ∼50 AU results in the largest super Earth populations, while both larger and smaller disk sizes result in the ice line producing more gas giants near 1 AU. This transition between typical planet class formed at the ice line at various disk radii confirms that planet formation is fundamentally linked to disk properties (in this case, disk size), and is a result that is only seen when dust evolution effects are included in our models. Additionally, we find that including radial dust drift results in the formation of more super Earths between 0.1 -1 AU, having shorter orbital radii than those produced in models where dust evolution effects are not included.

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“…Pinilla et al (2018) for a 0.1-0.2 M star. The samples of Andrews et al (2018a) and Long et al (2019) also contain a few low-mass stars, though at the moment there is no correlation between the sub-structure properties with the stellar properties (Huang et al 2018). At the moment it is difficult to say whether this is due to selection biases (for example Andrews et al 2018a targeted the brightest discs), the low number statistics (even combined, there are only a handful of stars in these samples below 0.5 M ) or if it is physical.…”

Section: Observational Implicationsmentioning

confidence: 99%

Planet gap opening across stellar masses

Sinclair

Rosotti

Juhász

et al. 2020

Monthly Notices of the Royal Astronomical Society

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Annular structures in proto-planetary discs, such as gaps and rings, are now ubiquitously found by high-resolution ALMA observations. Under the hypothesis that they are opened by planets, in this paper we investigate how the minimum planet mass needed to open a gap varies across different stellar host masses and distances from the star. The dependence on the stellar host mass is particularly interesting because, at least in principle, gap opening around low mass stars should be possible for lower mass planets, giving us a look into the young, low mass planet population. Using dusty hydrodynamical simulations, we find however the opposite behaviour, as a result of the fact that discs around low mass stars are geometrically thicker: gap opening around low mass stars can require more massive planets. Depending on the theoretical isochrone employed to predict the relationship between stellar mass and luminosity, the gap opening planet mass could also be independent of stellar mass, but in no case we find that gap opening becomes easier around low mass stars. This would lead to the expectation of a lower incidence of such structures in lower mass stars, since exoplanet surveys show that low mass stars have a lower fraction of giant planets. More generally, our study enables future imaging observations as a function of stellar mass to be interpreted using information on the mass vs. luminosity relations of the observed samples.

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Compact Disks in a High-resolution ALMA Survey of Dust Structures in the Taurus Molecular Cloud

Cited by 226 publications

References 116 publications

A Ringed Pole-on Outflow from DO Tauri Revealed by ALMA

A Ringed Pole-on Outflow from DO Tauri Revealed by ALMA

Formation of planetary populations − II. Effects of initial disc size and radial dust drift

Planet gap opening across stellar masses

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