High-resolution ALMA and <i>HST</i> images of q1 Eri: an asymmetric debris disc with an eccentric Jupiter

Lovell, Joshua B.; Marino, Sebastián; Wyatt, M. C.; Kennedy, Grant M.; MacGregor, Meredith A.; Stapelfeldt, K.; Dent, Bill; Krist, John; Matrà, Luca; Kral, Quentin; Panić, Olja; Pearce, Tim D.; Wilner, David J.

doi:10.1093/mnras/stab1678

Cited by 24 publications

(24 citation statements)

References 99 publications

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“…3.7). Such an asymmetry profile is found in several debris disc systems in the ALMA continuum, e.g., HR 8799 (Faramaz et al 2021) and q1 Eri (Lovell et al 2021).…”

Section: Hr 8799 and Other Planet Systems In Debris Discmentioning

confidence: 64%

Efficient planet formation by pebble accretion in ALMA rings

Jiang¹,

Ormel²

2022

Preprint

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In the past decade, ALMA observations have revealed that a large fraction of protoplanetary discs contains rings in the dust continuum. These rings are the locations where pebbles accumulate, which is beneficial for planetesimal formation and subsequent planet assembly. We investigate the viability of planet formation inside ALMA rings in which pebbles are trapped by either a Gaussian-shape pressure bump or by the strong dust backreaction. Planetesimals form at the midplane of the ring via streaming instability. By conducting N-body simulations, we study the growth of these planetesimals by collisional mergers and pebble accretion. Thanks to the high concentration of pebbles in the ring, the growth of planetesimals by pebble accretion becomes efficient as soon as they are born. We find that type-I migration plays a decisive role in the evolution of rings and planets. For discs where planets can migrate inward from the ring, a steady state is reached where the ring spawns ∼20𝑀 ⊕ planetary cores as long as rings are fed with materials from the outer disc. The ring acts as a long-lived planet factory and it can explain the "fine-tuned" optical depths of the observed dust rings in the DSHARP large program. In contrast, in the absence of a planet removal mechanism (migration), a single massive planet will form and destroy the ring. A wide and massive planetesimals belt will be left at the location of the planet-forming ring. Planet formation in rings may explain the mature planetary systems observed inside debris discs.

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“…3.7). Such an asymmetry profile is found in several debris disc systems in the ALMA continuum, e.g., HR 8799 (Faramaz et al 2021) and q1 Eri (Lovell et al 2021).…”

Section: Hr 8799 and Other Planet Systems In Debris Discmentioning

confidence: 64%

Efficient planet formation by pebble accretion in ALMA rings

Jiang¹,

Ormel²

2022

Preprint

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“…7), also show broad wings (though not convolved by a PSF or a beam), even for simulations without gas, while the inclinations of the particles are drawn from one normal distribution, suggesting that two populations might not be required to fully explain the ALMA observations. Lovell et al (2021) modeled ALMA observations of the disk around q 1 Eri, and found a scale height ℎ ∼ 0.05 (ℎ being the standard deviation of a Gaussian profile), corresponding to an aspect ratio of FWHM(𝑟 0 )/𝑟 0 ∼ 0.12, slightly larger than the values reported for the other disks above. Marino et al (2016) reported an upper limit for HD 181327, with an aspect ratio (using a Gaussian profile) that has to be smaller than 0.14, but the inclination of the disk around HD 181327 is not the most favorable to firmly constrain its vertical structure (though see Section 4.9 in Marino et al 2016 for a discussion on the impact of the radial width, vertical extent, and inclination).…”

Section: Vertical Scale Height At Millimeter Wavelengthsmentioning

confidence: 77%

The vertical structure of debris disks and the impact of gas

Olofsson,

Thébault,

Kral

et al. 2022

Preprint

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The vertical structure of debris disks provides clues about their dynamical evolution and the collision rate of the unseen planetesimals. Thanks to the ever-increasing angular resolution of contemporary instruments and facilities, we are beginning to constrain the scale height of a handful of debris disks, either at near-infrared or millimeter wavelengths. Nonetheless, this is often done for individual targets only. We present here the geometric modeling of eight disks close to edge-on, all observed with the same instrument (SPHERE) and using the same mode (dual-beam polarimetric imaging). Motivated by the presence of CO gas in two out of the eight disks, we then investigate the impact that gas can have on the scale height by performing N-body simulations including gas drag and collisions. We show that gas can quickly alter the dynamics of particles (both in the radial and vertical directions), otherwise governed by gravity and radiation pressure. We find that, in the presence of gas, particles smaller than a few tens of microns can efficiently settle toward the midplane at the same time as they migrate outward beyond the birth ring. For second generation gas (𝑀 gas ≤ 0.1 𝑀 ⊕ ), the vertical settling should be best observed in scattered light images compared to observations at millimeter wavelengths. But if the gas has a primordial origin (𝑀 gas ≥ 1 𝑀 ⊕ ), the disk will appear very flat both at near-infrared and sub-mm wavelengths. Finally, far beyond the birth ring, our results suggest that the surface brightness profile can be as shallow as ∼ −2.25.

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“…The ALMA data are from Lovell et al (2021) and show that the disc is asymmetric with a sharp inner edge. Lovell et al (2021) model this as a symmetric disc with a possible resonant clump, but they also show that a non-resonant, eccentric planet with a p e p = 2 − 4 au could instead drive the observed asymmetries. If the latter scenario applies, then these planet constraints agree with ours.…”

Section: Appendix A: System Datamentioning

confidence: 99%

Planet populations inferred from debris discs

Pearce

Launhardt

Ostermann

et al. 2022

A&A

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We know little about the outermost exoplanets in planetary systems because our detection methods are insensitive to moderate-mass planets on wide orbits. However, debris discs can probe the outer-planet population because dynamical modelling of observed discs can reveal properties of perturbing planets. We use four sculpting and stirring arguments to infer planet properties in 178 debris-disc systems from the ISPY, LEECH, and LIStEN planet-hunting surveys. Similar analyses are often conducted for individual discs, but we consider a large sample in a consistent manner. We aim to predict the population of wide-separation planets, gain insight into the formation and evolution histories of planetary systems, and determine the feasibility of detecting these planets in the near future. We show that a ‘typical’ cold debris disc likely requires a Neptune- to Saturn-mass planet at 10–100 au, with some needing Jupiter-mass perturbers. Our predicted planets are currently undetectable, but modest detection-limit improvements (e.g. from JWST) should reveal many such perturbers. We find that planets thought to be perturbing debris discs at late times are similar to those inferred to be forming in protoplanetary discs, so these could be the same population if newly formed planets do not migrate as far as currently thought. Alternatively, young planets could rapidly sculpt debris before migrating inwards, meaning that the responsible planets are more massive (and located farther inwards) than debris-disc studies assume. We combine self-stirring and size-distribution modelling to show that many debris discs cannot be self-stirred without having unreasonably high masses; planet- or companion-stirring may therefore be the dominant mechanism in many (perhaps all) debris discs. Finally, we provide catalogues of planet predictions and identify promising targets for future planet searches.

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High-resolution ALMA and HST images of q1 Eri: an asymmetric debris disc with an eccentric Jupiter

Cited by 24 publications

References 99 publications

Efficient planet formation by pebble accretion in ALMA rings

Efficient planet formation by pebble accretion in ALMA rings

The vertical structure of debris disks and the impact of gas

Planet populations inferred from debris discs

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