ALMA 870 μm continuum observations of HD 100546

Fedele, D.; Toci, Claudia; Maud, L. T.; Lodato, Giuseppe

doi:10.1051/0004-6361/202141278

Cited by 26 publications

(35 citation statements)

References 69 publications

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“…Pyerin et al 2021). Recent modeling suggests a 8.5 M Jup planet at 110 au (see Figure 4) and predicts locally diminished gas and millimeter dust surface densities (Fedele et al 2021). Pyerin et al (2021) instead find evidence of a 3 M Jup planet at 143 au, which places the temperature bump interior to, and not radially coincident with, the proposed planet location.…”

Section: Temperature Substructuresmentioning

confidence: 93%

“…The radial locations of dust substructures indicated for the HD 100546 disk are approximate, since the location of dust features differs by a few tens of astronomical units along different projections due to the azimuthally asymmetric dust emission in this source (Pineda et al 2019;Pérez et al 2020;Fedele et al 2021). The dip in the emission surface of the HD 100546 disk is coincident with the inner edge of a wide (∼40-150 au) continuum gap (Pineda et al 2019;Fedele et al 2021). In CI Tau, the vertical dip in CO emitting heights also aligns with a millimeter dust gap.…”

Section: Vertical Substructures and Comparison With Millimeter Contin...mentioning

confidence: 96%

“…While we find a smoothly varying CO emission surface at these radii, a relatively wide vertical dip is present in the emitting heights a few tens of au exterior to this KPS. The proposed locations of two Jupitermass planets, one at 15 au and another at 110 au, from smoothed-particle-hydrodynamical simulations (Fedele et al 2021; but see Pyerin et al 2021 for alternate predictions of planet radial locations at 13 au and 143 au) are located at the inner and outermost edges, respectively, of where we constrained the CO emission surface. Similar to the KPS in the CI Tau disk, we are unable to determine if any corresponding vertical substructures are present in the HD 100546 disk at or near these radii.…”

Section: Notesmentioning

confidence: 99%

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CO Line Emission Surfaces and Vertical Structure in Midinclination Protoplanetary Disks

Law

Crystian

Teague

et al. 2022

ApJ

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High spatial resolution CO observations of midinclination (≈30°–75°) protoplanetary disks offer an opportunity to study the vertical distribution of CO emission and temperature. The asymmetry of line emission relative to the disk major axis allows for a direct mapping of the emission height above the midplane, and for optically thick, spatially resolved emission in LTE, the intensity is a measure of the local gas temperature. Our analysis of Atacama Large Millimeter/submillimeter Array archival data yields CO emission surfaces, dynamically constrained stellar host masses, and disk atmosphere gas temperatures for the disks around the following: HD 142666, MY Lup, V4046 Sgr, HD 100546, GW Lup, WaOph 6, DoAr 25, Sz 91, CI Tau, and DM Tau. These sources span a wide range in stellar masses (0.50–2.10 M ⊙), ages (∼0.3–23 Myr), and CO gas radial emission extents (≈200–1000 au). This sample nearly triples the number of disks with mapped emission surfaces and confirms the wide diversity in line emitting heights (z/r ≈ 0.1 to ≳0.5) hinted at in previous studies. We compute the radial and vertical CO gas temperature distributions for each disk. A few disks show local temperature dips or enhancements, some of which correspond to dust substructures or the proposed locations of embedded planets. Several emission surfaces also show vertical substructures, which all align with rings and gaps in the millimeter dust. Combining our sample with literature sources, we find that CO line emitting heights weakly decline with stellar mass and gas temperature, which, despite large scatter, is consistent with simple scaling relations. We also observe a correlation between CO emission height and disk size, which is due to the flared structure of disks. Overall, CO emission surfaces trace ≈2–5× gas pressure scale heights (Hg) and could potentially be calibrated as empirical tracers of Hg.

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Section: Temperature Substructuresmentioning

confidence: 93%

Section: Vertical Substructures and Comparison With Millimeter Contin...mentioning

confidence: 96%

Section: Notesmentioning

confidence: 99%

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CO Line Emission Surfaces and Vertical Structure in Midinclination Protoplanetary Disks

Law

Crystian

Teague

et al. 2022

ApJ

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“…Interactions with planets seem to reproduce at least some observed substructures (e.g., Pinilla et al 2012;Dipierro et al 2015;Dong et al 2015;Zhang et al 2018;Hammer et al 2021;Rodenkirch et al 2021;Fedele et al 2021), including the remarkable case of PDS70 where such planets have been observed (Keppler et al 2018;Müller et al 2018;Wagner et al 2018;Haffert et al 2019). As in PDS70, super-Jovian-mass planets are often invoked to reproduce the dust continuum observations by the Atacama Large Millimeter/submillimeter Array (ALMA; Bae et al 2018;Long et al 2018;Lodato et al 2019), though such planets have small occurrence rates as shown by direct imaging campaigns (Bowler & Nielsen 2018).…”

Section: Introductionmentioning

confidence: 98%

Substructures in Protoplanetary Disks Imprinted by Compact Planetary Systems

Garrido-Deutelmoser

Petrovich

Krapp

et al. 2022

ApJ

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The substructures observed in protoplanetary disks may be the signposts of embedded planets carving gaps or creating vortices. The inferred masses of these planets often fall in the Jovian regime despite their low abundance compared to lower-mass planets, partly because previous works often assume that a single substructure (a gap or vortex) is caused by a single planet. In this work, we study the possible imprints of compact systems composed of Neptune-like planets (∼10–30 M ⊕) and show that long-standing vortices are a prevalent outcome when their interplanetary separation (Δa) falls below ∼8 times H p—the average disk’s scale height at the planet’s locations. In simulations where a single planet is unable to produce long-lived vortices, two-planet systems can preserve them for at least 5000 orbits in two regimes: (i) fully shared density gaps with elongated vortices around the stable Lagrange points L 4 and L 5 for the most compact planet pairs (Δa ≲ 4.6 H p), and (ii) partially shared gaps for more widely spaced planets (Δa ∼ 4.6–8 H p) forming vortices in a density ring between the planets through the Rossby wave instability. The latter case can produce vortices with a wide range of aspect ratios down to ∼3 and can occur for planets captured into the 3:2 (2:1) mean-motion resonances for disks’ aspects ratios of h ≳ 0.033 (h ≳ 0.057). We suggest that their long lifetimes are sustained by the interaction of spiral density waves launched by the neighboring planets. Overall, our results show that the distinguishing imprint of compact systems with Neptune-mass planets are long-lived vortices inside the density gaps, which in turn are shallower than single-planet gaps for a fixed gap width.

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“…Interactions with planets seem to reproduce at least some observed substructures (e.g., Pinilla et al 2012;Dipierro et al 2015;Dong et al 2015;Zhang et al 2018;Hammer et al 2021;Rodenkirch et al 2021;Fedele et al 2021), including the remarkable case of PDS70 where such planets have been observed (Keppler et al 2018;Müller et al 2018;Wagner et al 2018;Haffert et al 2019). As in PDS70, super Jovian-mass planets are often invoked to reproduce the dust continuum observations by ALMA (Long et al 2018;Bae et al 2018;Lodato et al 2019), though such planets have small occurrence rates as shown by direct imaging campaigns (Bowler & Nielsen 2018); a potential tension that is alleviated if the planets eventually migrate inwards (van der Marel & Mulders 2021).…”

Section: Introductionmentioning

confidence: 99%

Substructures in protoplanetary disks imprinted by compact planetary systems

Garrido-Deutelmoser,

Petrovich,

Krapp

et al. 2022

Preprint

View full text Add to dashboard Cite

The substructures observed in protoplanetary disks may be the signposts of embedded planets carving gaps or creating vortices. The inferred masses of these planets often fall in the Jovian regime despite their low abundance compared to lower-mass planets, partly because previous works often assume that a single substructure (a gap or vortex) is caused by a single planet. In this work, we study the possible imprints of compact systems composed of Neptune-like planets (∼ 10 − 30 M ⊕ ) and show that longstanding vortices are a prevalent outcome when their inter-planetary separation (∆a) falls below ∼ 8 times H p -the average disk's scale height at the planets locations. In simulations where a single planet is unable to produce long-lived vortices, two-planet systems can preserve them for at least 5, 000 orbits in two regimes: i) fully-shared density gaps with elongated vortices around the stable Lagrange points L 4 and L 5 for the most compact planet pairs (∆a 4.6 H p ); ii) partially-shared gaps for more widely spaced planets (∆a ∼ 4.6 − 8 H p ) forming vortices in a density ring between the planets through the Rossby wave instability. The latter case can produce vortices with a wide range of aspect ratios down to ∼ 3 and can occur for planets captured into the 3:2 (2:1) mean-motion resonances for disk's aspects ratios of h 0.033 (h 0.057). We suggest that their long lifetimes are sustained by the interaction of spiral density waves launched by the neighboring planets. Overall, our results show that distinguishing imprint of compact systems with Neptune-mass planets are long-lived vortices inside the density gaps, which in turn are shallower than single-planet gaps for a fixed gap width.

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ALMA 870 μm continuum observations of HD 100546

Cited by 26 publications

References 69 publications

CO Line Emission Surfaces and Vertical Structure in Midinclination Protoplanetary Disks

CO Line Emission Surfaces and Vertical Structure in Midinclination Protoplanetary Disks

Substructures in Protoplanetary Disks Imprinted by Compact Planetary Systems

Substructures in protoplanetary disks imprinted by compact planetary systems

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