ALMA survey of Lupus class III stars: Early planetesimal belt formation and rapid disc dispersal

Lovell, Joshua B.; Wyatt, M. C.; Ansdell, Megan; Kama, M.; Kennedy, Grant M.; Manara, C. F.; Marino, Sebastián; Matrà, Luca; Rosotti, Giovanni; Tazzari, Marco; Testi, L.; Williams, Jonathan P.

doi:10.1093/mnras/staa3335

Cited by 25 publications

(22 citation statements)

References 133 publications

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“…Based on their observational results, they suggest that there is rapid protoplanetary disk mm-dust dispersal and evolution such that planetesimals form within ∼2 Myr. Their conclusions suggest that some Lupus disks aged 1-3 Myr are already debris disks and will evolve into objects similar to the currently observed debris disk sample (see Figure 10 in Lovell et al (2021)). Therefore, we aim to further expand on our understanding of the role of Class III disks in the evolutionary process bridging the gap between the protoplanetary and debris disk phases.…”

Section: Introductionmentioning

confidence: 64%

“…It is important to note here that previous works comparing dust masses of protoplanetary disks with debris disks reported a significant decrease in dust mass of 2-3 orders of magnitude between these two populations (Wyatt 2008;Panić et al 2013;Hardy et al 2015), which they interpret as rapid photoevaporative clearing (Clarke et al 2001). However, these studies mostly included pre-ALMA measurements of protoplanetary disks, which did not have the sensitivity of the more recent ALMA surveys (Ansdell et al 2016;Barenfeld et al 2016;Williams et al 2019;Lovell et al 2021). The current data reveal that even in the protoplanetary disk phase the mass in millimeter grains has already declined to levels comparable to those measured in debris disks.…”

Section: Disk Evolutionmentioning

confidence: 72%

“…However, a series of YSOs, while detected at shorter infrared wavelengths (3 to 12 µm -IRAC1/WISE1 to IRAC4/WISE3 band) are lacking 22-24 µm (MIPS1/WISE4) detections, given that these are members of young star-forming regions, we define these as Class III-shortλ (Class III-sλ). We avoid using the term diskless or bare photospheres as recent studies (Lovell et al 2021) demonstrate that evolved disks can have very faint and low mass disks.…”

Section: Classificationmentioning

confidence: 99%

“…Hardy et al 2015;Barenfeld et al 2016;Williams et al 2019). Recently, Lovell et al (2021) reported new ALMA observations of 30 Class III YSOs associated with the Lupus star forming regions. Although they obtained very deep sensitivities for each target, only 4 Class III objects were detected.…”

Section: Introductionmentioning

confidence: 99%

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Bridging the gap between protoplanetary and debris disks: separate evolution of millimeter and micrometer-sized dust

Michel,

van der Marel,

Matthews

2021

Preprint

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The connection between the nature of a protoplanetary disk and that of a debris disk is not well understood. Dust evolution, planet formation, and disk dissipation likely play a role in the processes involved. We aim to reconcile both manifestations of dusty circumstellar disks through a study of optically thin Class III disks and how they correlate to younger and older disks. In this work, we collect literature and ALMA archival millimeter fluxes for 85 disks (8%) of all Class III disks across nearby star-forming regions. We derive millimeter-dust masses and compare these with Class II and debris disk samples in the context of excess infrared luminosity, accretion rate, and age. The mean dust mass M dust of Class III disks is 0.29±0.19 M ⊕ . We propose a new evolutionary scenario wherein radial drift is very efficient for non-structured disks during the Class II phase resulting in a rapid decrease of M dust , whereas disk dissipation is a more gradual process. We find long infrared protoplanetary disk timescales of ∼9-10 Myr, which are also consistent with slow disk evolution. Finally, in structured disks, the presence of dust traps allows for the formation of planetesimal belts at large radii, such as those observed in debris disks. We propose that structured disks are thus directly connected to debris disks in one evolutionary pathway, in contrast to radial drift dominated disks which evolve to near diskless stars. These results set the scene for a novel view of disk evolution.

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Section: Introductionmentioning

confidence: 64%

Section: Disk Evolutionmentioning

confidence: 72%

Section: Classificationmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Bridging the gap between protoplanetary and debris disks: separate evolution of millimeter and micrometer-sized dust

Michel,

van der Marel,

Matthews

2021

Preprint

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“…This would result in very long dispersal times, much longer than the typically observed value of few Myr (Hernández et al 2008). The fact that Class III objects show mm emission similar to that of field debris disks (Lovell et al 2021;Michel et al 2021), suggests that disks may need to dissipate very fast, much faster than the ages of the ones we observe in the surviving Class II populations. The most likely candidates for these fast dissipation processes are photoevaporation or planet formation.…”

Section: Disk Dispersal Processesmentioning

confidence: 67%

The protoplanetary disk population in the rho-Ophiuchi region L1688 and the time evolution of Class II YSOs

Testi,

Natta,

Manara

et al. 2022

Preprint

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Context. Planets form during the first few Myr of the evolution of the star-disk system, possibly before the end of the embedded phase. The properties of the very young disks and the following evolution reflects the presence and properties of their planetary content. Aims. We present a study of the Class II/ F disk population in L1688, the densest and youngest region of star formation in Ophiuchus, and we compare it with other well-known nearby regions of different age, namely Lupus, Chamaeleon I, Corona Australis, Taurus and Upper Scorpius. Methods. We select our L1688 sample using a combination of criteria (available ALMA data, membership from Gaia, optical/near-IR spectroscopy) and determine stellar and disk properties, specifically stellar mass (M ), average population age, mass accretion rate ( Ṁacc ) and disk dust mass (M dust ). We apply the same procedure in a consistent way to the other regions. Results. a) In L1688 the relations between Ṁacc and M , M dust and M , and Ṁacc and M dust have a roughly linear trend with slopes 1.8-1.9 for the first two relations and ∼ 1 for the third, similarly to what found in the other regions. b) When ordered according to the characteristic age of each region, which range from ∼ 0.5 to ∼ 5 Myr, Ṁacc decreases as t −1 , when corrected for the different stellar mass content; M dust follows roughly the same trend between 0.5 and 5 Myr, but has an increase of a factor ∼ 3 at ages of 2-3 Myr. We suggest that this could result from an earlier planet formation, followed by collisional fragmentation that temporarily replenishes the millimeter-size grain population. c) The dispersion of Ṁacc and M dust around the best-fitting relation with M , as well as that of Ṁacc versus M dust are equally large. When adding all the regions together to increase the statistical significance, we find that the dispersions have continuous distributions with a log-normal shape and similar width (∼ 0.8 dex). Conclusions. This detailed study of L1688 confirms and extends to a younger age the general picture of Class II/F disk properties. The amount of dust observed at ∼1Myr is not sufficient to assemble the majority of planetary systems, which suggests an earlier planetary cores formation. The dust mass traces to a large extent the disk gas mass evolution, even if the ratio M dust /M disk at the earliest age (0.5-1 Myr) is not known. Two properties remain puzzling: the steep dependence of Ṁacc and M dust on M and the cause of the large dispersion in the three relations analyzed in this paper, in particular the one of the Ṁacc versus M dust relation.

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The formation of planetary systems with SPICA

Kamp

Honda

Nomura

et al. 2021

Publ. Astron. Soc. Aust.

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In this era of spatially resolved observations of planet-forming disks with Atacama Large Millimeter Array (ALMA) and large ground-based telescopes such as the Very Large Telescope (VLT), Keck, and Subaru, we still lack statistically relevant information on the quantity and composition of the material that is building the planets, such as the total disk gas mass, the ice content of dust, and the state of water in planetesimals. SPace Infrared telescope for Cosmology and Astrophysics (SPICA) is an infrared space mission concept developed jointly by Japan Aerospace Exploration Agency (JAXA) and European Space Agency (ESA) to address these questions. The key unique capabilities of SPICA that enable this research are (1) the wide spectral coverage $10{-}220\,\mu\mathrm{m}$ , (2) the high line detection sensitivity of $(1{-}2) \times 10^{-19}\,\mathrm{W\,m}^{-2}$ with $R \sim 2\,000{-}5\,000$ in the far-IR (SAFARI), and $10^{-20}\,\mathrm{W\,m}^{-2}$ with $R \sim 29\,000$ in the mid-IR (SPICA Mid-infrared Instrument (SMI), spectrally resolving line profiles), (3) the high far-IR continuum sensitivity of 0.45 mJy (SAFARI), and (4) the observing efficiency for point source surveys. This paper details how mid- to far-IR infrared spectra will be unique in measuring the gas masses and water/ice content of disks and how these quantities evolve during the planet-forming period. These observations will clarify the crucial transition when disks exhaust their primordial gas and further planet formation requires secondary gas produced from planetesimals. The high spectral resolution mid-IR is also unique for determining the location of the snowline dividing the rocky and icy mass reservoirs within the disk and how the divide evolves during the build-up of planetary systems. Infrared spectroscopy (mid- to far-IR) of key solid-state bands is crucial for assessing whether extensive radial mixing, which is part of our Solar System history, is a general process occurring in most planetary systems and whether extrasolar planetesimals are similar to our Solar System comets/asteroids. We demonstrate that the SPICA mission concept would allow us to achieve the above ambitious science goals through large surveys of several hundred disks within $\sim\!2.5$ months of observing time.

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ALMA survey of Lupus class III stars: Early planetesimal belt formation and rapid disc dispersal

Cited by 25 publications

References 133 publications

Bridging the gap between protoplanetary and debris disks: separate evolution of millimeter and micrometer-sized dust

Bridging the gap between protoplanetary and debris disks: separate evolution of millimeter and micrometer-sized dust

The protoplanetary disk population in the rho-Ophiuchi region L1688 and the time evolution of Class II YSOs

The formation of planetary systems with SPICA

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