Planet gap opening across stellar masses

Sinclair, Catriona A; Rosotti, Giovanni; Juhász, A.; Clarke, C. J.

doi:10.1093/mnras/staa539

Cited by 21 publications

(17 citation statements)

References 86 publications

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“…ALMA Cycle 3 observations of CIDA 1 revealed for the first time a dust-depleted inner cavity around a VLMS, with a ring with maximum brightness at ∼20 au (Pinilla et al 2018a), which is a typical feature of the transition disk (TD) population. The observed structure in CIDA 1 may suggest that cavity opening processes are common in millimeter-bright disks independent of the central star mass, including VLMSs (Pinilla et al 2018b(Pinilla et al , 2020Sinclair et al 2020).…”

Section: A122 Page 1 Of 13mentioning

confidence: 93%

A bright inner disk and structures in the transition disk around the very low-mass star CIDA 1

Pinilla

Kurtovic

Benisty

et al. 2021

A&A

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The frequency of Earth-sized planets in habitable zones appears to be higher around M-dwarfs, making these systems exciting laboratories to investigate planet formation. Observations of protoplanetary disks around very low-mass stars and brown dwarfs remain challenging and little is known about their properties. The disk around CIDA 1 (~0.1–0.2 M⊙) is one of the very few known disks that host a large cavity (20 au radius in size) around a very low-mass star. We present new ALMA observations at Band 7 (0.9 mm) and Band 4 (2.1 mm) of CIDA 1 with a resolution of ~0.05″ × 0.034″. These new ALMA observations reveal a very bright and unresolved inner disk, a shallow spectral index of the dust emission (~2), and a complex morphology of a ring located at 20 au. We also present X-shooter (VLT) observations that confirm the high accretion rate of CIDA 1 of Ṁacc = 1.4 × 10−8 M⊙ yr−1. This high value of Ṁacc, the observed inner disk, and the large cavity of 20 au exclude models of photo-evaporation to explain the observed cavity. When comparing these observations with models that combine planet–disk interaction, dust evolution, and radiative transfer, we exclude planets more massive than 0.5 MJup as the potential origin of the large cavity because with these it is difficult to maintain a long-lived and bright inner disk. Even in this planet mass regime, an additional physical process may be needed to stop the particles from migrating inwards and to maintain a bright inner disk on timescales of millions of years. Such mechanisms include a trap formed by a very close-in extra planet or the inner edge of a dead zone. The low spectral index of the disk around CIDA 1 is difficult to explain and challenges our current dust evolution models, in particular processes like fragmentation, growth, and diffusion of particles inside pressure bumps.

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Section: A122 Page 1 Of 13mentioning

confidence: 93%

A bright inner disk and structures in the transition disk around the very low-mass star CIDA 1

Pinilla

Kurtovic

Benisty

et al. 2021

A&A

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“…Pinilla et al (2018a) have thus far reported the lowest mass star with a resolved large dust cavity (radius ∼20 au) in the disk around the M 4.5 star CIDA 1. In the context of planets creating such a cavity, it has been shown that a high planet-to-stellar mass ratio is needed to open a gap and trap particles in disks around VLMS, because in these cases, the disk scale height at a given location is higher than in moderate or high mass stars (Pinilla et al 2017a;Sinclair et al 2020). In a typical disk around a VLMS as CIDA 1, at least a Saturn-mass planet is needed to open a gap in the disk.…”

Section: Introductionmentioning

confidence: 99%

Size and structures of disks around very low mass stars in the Taurus star-forming region

Kurtovic

Pinilla

Long

et al. 2021

A&A

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Context. The discovery of giant planets orbiting very low mass stars (VLMS) and the recent observed substructures in disks around VLMS is challenging planet formation models. Specifically, radial drift of dust particles is a catastrophic barrier in these disks, which prevents the formation of planetesimals and therefore planets. Aims. We aim to estimate if structures, such as cavities, rings, and gaps, are common in disks around VLMS and to test models of structure formation in these disks. We also aim to compare the radial extent of the gas and dust emission in disks around VLMS, which can give us insight about radial drift. Methods. We studied six disks around VLMS in the Taurus star-forming region using ALMA Band 7 (~340 GHz) at a resolution of ~0.1″. The targets were selected because of their high disk dust content in their stellar mass regime. Results. Our observations resolve the disk dust continuum in all disks. In addition, we detect the 12CO (J = 3−2) emission line in all targets and 13CO (J = 3−2) in five of the six sources. The angular resolution allows the detection of dust substructures in three out of the six disks, which we studied by using UV-modeling. Central cavities are observed in the disks around stars MHO 6 (M 5.0) and CIDA 1 (M 4.5), while we have a tentative detection of a multi-ringed disk around J0433. We estimate that a planet mass of ~0.1 MJup or ~0.4 MSaturn is required for a single planet to create the first gap in J0433. For the cavities of MHO 6 and CIDA 1, a Saturn-mass planet (~0.3 MJup) is required. The other three disks with no observed structures are the most compact and faintest in our sample, with the radius enclosing 90% of the continuum emission varying between ~13 and 21 au. The emission of 12CO and 13CO is more extended than the dust continuum emission in all disks of our sample. When using the 12CO emission to determine the gas disk extension Rgas, the ratio of Rgas∕Rdust in our sample varies from 2.3 to 6.0. One of the disks in our sample, CIDA 7, has the largest Rgas∕Rdust ratio observed so far, which is consistent with models of radial drift being very efficient around VLMS in the absence of substructures. Conclusions. Given our limited angular resolution, substructures were only directly detected in the most extended disks, which represent 50% of our sample, and there are hints of unresolved structured emission in one of the bright smooth sources. Our observations do not exclude giant planet formation on the substructures observed. A comparison of the size and luminosity of VLMS disks with their counterparts around higher mass stars shows that they follow a similar relation.

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“…At inner and outer boundaries, the gas velocities and densities are fixed to the initial steady-state value while the dust has an open inner boundary (Meru et al 2019;Sinclair et al 2020). We adopt the damping procedure (de Val-Borro et al 2006) to avoid artificial wave reflection.…”

Section: Numerical Setupmentioning

confidence: 99%

Wide Dust Gaps in Protoplanetary Disks Induced by Eccentric Planets: A Mass-Eccentricity Degeneracy

Chen,

Wang,

et al. 2021

Preprint

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The tidal perturbation of embedded protoplanets on their natal disks has been widely attributed to be the cause of gap-ring structures in sub-mm images of protoplanetary disks around T Tauri stars. Numerical simulations of this process have been used to propose scalings of characteristic dust gap width/gap-ring distance with respect to planet mass. Applying such scalings to analyze observed gap samples yields a continuous mass distribution for a rich population of hypothetical planets in the range of several Earth to Jupiter masses. In contrast, the conventional core-accretion scenario of planet formation predicts a bi-modal mass function due to 1) the onset of runaway gas accretion above ∼20 Earth masses and 2) suppression of accretion induced by gap opening. Here we examine the dust disk response to the tidal perturbation of eccentric planets as a possible resolution of this paradox. Based on simulated gas and dust distributions, we show the gap-ring separation of Neptune-mass planets with small eccentricities might become comparable to that induced by Saturn-mass planets on circular orbits. This degeneracy may obliterate the discrepancy between the theoretical bi-modal mass distribution and the observed continuous gap width distribution. Despite damping due to planet-disk interaction, modest eccentricity may be sustained either in the outer regions of relatively thick disks or through resonant excitation among multiple super Earths. Moreover, the ring-like dust distribution induced by planets with small eccentricities is axisymmetric even in low viscosity environments, consistent with the paucity of vortices in ALMA images.

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Planet gap opening across stellar masses

Cited by 21 publications

References 86 publications

A bright inner disk and structures in the transition disk around the very low-mass star CIDA 1

A bright inner disk and structures in the transition disk around the very low-mass star CIDA 1

Size and structures of disks around very low mass stars in the Taurus star-forming region

Wide Dust Gaps in Protoplanetary Disks Induced by Eccentric Planets: A Mass-Eccentricity Degeneracy

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