Observability of forming planets and their circumplanetary discs – I. Parameter study for ALMA

Szulágyi, J.; Plas, G. van der; Meyer, M. R.; Pohl, A.; Quanz, Sascha P.; Mayer, Lucio; Daemgen, S.; Tamburello, Valentina

doi:10.1093/mnras/stx2602

Cited by 52 publications

(58 citation statements)

References 70 publications

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“…• The CPD mass upper limit is enough to be incompatible with several planet accretion models, while synthetic observations of numerical simulation by Szulágyi et al (2018) provide a CPD flux similar to the upper limit reported here. Gas-starved models are also still compatible.…”

Section: Discussionsupporting

confidence: 59%

High-resolution ALMA Observations of HD 100546: Asymmetric Circumstellar Ring and Circumplanetary Disk Upper Limits

Pineda

Szulágyi

Quanz

et al. 2019

ApJ

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We present long baseline Atacama Large Millimeter/submillimeter Array (ALMA) observations of the 870 µm dust continuum emission and CO (3-2) from the protoplanetary disk around the Herbig Ae/Be star HD 100546, which is one of the few systems claimed to have two young embedded planets. These observations achieve a resolution of 4 au (3.8 mas), an rms noise of 66 µJy beam −1 , and reveal an asymmetric ring between ∼20-40 au with largely optically thin dust continuum emission. This ring is well fit by two concentric and overlapping Gaussian rings of different widths and a Vortex. In addition, an unresolved component is detected at a position consistent with the central star, which may trace the central inner disk (<2 au in radius). We report a lack of compact continuum emission at the positions of both claimed protoplanets. We use this result to constrain the circumplanetary disk (CPD) mass and size of 1.44 M ⊕ and 0.44 au in the optically thin and thick regime, respectively, for the case of the previously directly imaged protoplanet candidate at ∼55 au (HD100546 b). We compare these empirical CPD constraints to previous numerical simulations. This suggests that HD100546 b is inconsistent with several planet accretion models, while gas-starved models are also still compatible. We estimate the planetary mass as 1.65 M J by using the relation between planet, circumstellar, and circumplanetary masses derived from numerical simulations. Finally, the CO integrated intensity map shows a possible spiral arm feature that would match the spiral features identified in Near-Infrared scattered light polarized emission, which suggests a real spiral feature in the disk surface that needs to be confirmed with further observations.

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Section: Discussionsupporting

confidence: 59%

High-resolution ALMA Observations of HD 100546: Asymmetric Circumstellar Ring and Circumplanetary Disk Upper Limits

Pineda

Szulágyi

Quanz

et al. 2019

ApJ

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“…Marley et al 2007;Mordasini et al 2012;Mordasini 2013;Baruteau et al 2016). The estimated temperatures are similar to the temperatures of the accretion shock around planets formed by core accretion (Marleau et al 2017(Marleau et al , 2019Szulágyi 2017;Szulágyi et al 2018;Szulágyi & Mordasini 2017) and therefore their circumplanetary discs are also expected to be relatively hot. These high temperatures contradict the results of the disc instability model presented in , as in the simulations presented here we were able to follow the collapse of a fragment at much higher densities and capture the formation of the first and second core.…”

Section: The Properties Of Protoplanets Formed Around M Dwarfs By Dissupporting

confidence: 55%

Planet formation around M dwarfs via disc instability

Mercer

Stamatellos

2020

A&A

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Context. Around 30 per cent of the observed exoplanets that orbit M dwarf stars are gas giants that are more massive than Jupiter. These planets are prime candidates for formation by disc instability. Aims. We want to determine the conditions for disc fragmentation around M dwarfs and the properties of the planets that are formed by disc instability. Methods. We performed hydrodynamic simulations of M dwarf protostellar discs in order to determine the minimum disc mass required for gravitational fragmentation to occur. Different stellar masses, disc radii, and metallicities were considered. The mass of each protostellar disc was steadily increased until the disc fragmented and a protoplanet was formed. Results. We find that a disc-to-star mass ratio between ~0.3 and ~0.6 is required for fragmentation to happen. The minimum mass at which a disc fragment increases with the stellar mass and the disc size. Metallicity does not significantly affect the minimum disc fragmentation mass but high metallicity may suppress fragmentation. Protoplanets form quickly (within a few thousand years) at distances around ~50 AU from the host star, and they are initially very hot; their centres have temperatures similar to the ones expected at the accretion shocks around planets formed by core accretion (up to 12 000 K). The final properties of these planets (e.g. mass and orbital radius) are determined through long-term disc-planet or planet–planet interactions. Conclusions. Disc instability is a plausible way to form gas giant planets around M dwarfs provided that discs have at least 30% the mass of their host stars during the initial stages of their formation. Future observations of massive M dwarf discs or planets around very young M dwarfs are required to establish the importance of disc instability for planet formation around low-mass stars.

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“…A timespan of about 1 week would be enough to observe the proper motion of a circumplanetary disk detected with the same signal-to-noise ratio but at an orbital radius of 1 au. Similar predictions for the expected circumplanetary disk fluxes at these wavelengths are derived from the α−models of Zhu et al (2017), whereas significantly brighter fluxes are obtained if adiabatic compression due to the accretion process is the main heating mechanism in these systems (Szulágyi et al 2016(Szulágyi et al , 2017. Brighter circumplanetary disks, up to ∼ 100 µJy at 3 mm, are expected also around planets further from the star, where the Hill radius, and therefore the expected disk radius as well, are larger .…”

Section: Different Distances From Earthsupporting

confidence: 72%

Investigating the Early Evolution of Planetary Systems with ALMA and the Next Generation Very Large Array

Ricci

Liu

Isella

et al. 2018

ApJ

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We investigate the potential of the Atacama Large Millimeter/submillimeter Array (ALMA) and the Next Generation Very Large Array (ngVLA) to observe substructures in nearby young disks which are due to the gravitational interaction between disk material and planets close to the central star. We simulate the gas and dust dynamics in the disk using the LA-COMPASS hydrodynamical code. We generate synthetic images for the dust continuum emission at sub-millimeter to centimeter wavelengths and simulate ALMA and ngVLA observations. We explore the parameter space of some of the main disk and planet properties that would produce substructures that can be visible with ALMA and the ngVLA. We find that ngVLA observations with an angular resolution of 5 milliarcsec at 3 mm can reveal and characterize gaps and azimuthal asymmetries in disks hosting planets with masses down to ≈ 5M ⊕ ≈ 1 − 5 au from a Solar-like star in the closest star forming regions, whereas ALMA can detect gaps down to planetary masses of ≈ 20 M ⊕ at 5 au. Gaps opened by super-Earth planets with masses ≈ 5 − 10M ⊕ are detectable by the ngVLA in the case of disks with low viscosity (α ∼ 10 −5 ) and low pressure scale height (h ≈ 0.025 au at 5 au). The ngVLA can measure the proper motion of azimuthal asymmetric structures associated with the disk-planet interaction, as well as possible circumplanetary disks on timescales as short as one to a few weeks for planets at 1 − 5 au from the star.

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Observability of forming planets and their circumplanetary discs – I. Parameter study for ALMA

Cited by 52 publications

References 70 publications

High-resolution ALMA Observations of HD 100546: Asymmetric Circumstellar Ring and Circumplanetary Disk Upper Limits

High-resolution ALMA Observations of HD 100546: Asymmetric Circumstellar Ring and Circumplanetary Disk Upper Limits

Planet formation around M dwarfs via disc instability

Investigating the Early Evolution of Planetary Systems with ALMA and the Next Generation Very Large Array

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