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ALMA survey of lupus class III stars : early planetesimal belt formation and rapid disk dispersal
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Lovell, J. B., Wyatt, M. C., Ansdell, M., Kama, M., Kennedy, Grant M., Manara, C. F., Marino, S., Matrà, L., Rosotti, G., Tazzari, M., Testi, L. and Williams, J. P. (2021) ALMA survey of lupus class III stars : early planetesimal belt formation and rapid disk dispersal. Monthly Notices of the Royal Astronomical Society, 500 (4). pp. 4878-4900. doi:10.1093/mnras/staa3335
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WRAP-ALMA-survey-lupus-class-III-stars-planetesimal-belt-rapid-Kennedy-2020.pdf - Accepted Version - Requires a PDF viewer. Download (6Mb) | Preview |
Official URL: http://dx.doi.org/10.1093/mnras/staa3335
Abstract
Class III stars are those in star forming regions without large non-photospheric infrared emission, suggesting recent dispersal of their protoplanetary disks. We observed 30 class III stars in the 1-3 Myr Lupus region with ALMA at ∼856μm, resulting in 4 detections that we attribute to circumstellar dust. Inferred dust masses are 0.036 - 0.093M⊕, ∼1 order of magnitude lower than any previous measurements; one disk is resolved with radius ∼80 au. Two class II sources in the field of view were also detected, and 11 other sources, consistent with sub-mm galaxy number counts. Stacking non-detections yields a marginal detection with mean dust mass ∼0.0048M⊕. We searched for gas emission from the CO J=3-2 line, and present its detection to NO Lup inferring a gas mass (4.9 ± 1.1) × 10-5 M⊕ and gas-to-dust ratio 1.0 ± 0.4. Combining our survey with class II sources shows a gap in the disk mass distribution from 0.09 - 2M⊕ for >0.7M☉ Lupus stars, evidence of rapid dispersal of mm-sized dust from protoplanetary disks. The class III disk mass distribution is consistent with a population model of planetesimal belts that go on to replenish the debris disks seen around main sequence stars. This suggests that planetesimal belt formation does not require long-lived protoplanetary disks, i.e., planetesimals form within ∼2 Myr. While all 4 class III disks are consistent with collisional replenishment, for two the gas and/or mid-IR emission could indicate primordial circumstellar material in the final stages of protoplanetary disk dispersal. Two class III stars without sub-mm detections exhibit hot emission that could arise from ongoing planet formation processes inside ∼1 au.
| Item Type: | Journal Article | |||||||||||||||||||||||||||
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| Subjects: | Q Science > QB Astronomy Q Science > QC Physics |
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| Divisions: | Faculty of Science > Physics | |||||||||||||||||||||||||||
| Library of Congress Subject Headings (LCSH): | Circumstellar matter , Planetary systems, Interferometry, Disks (Astrophysics) | |||||||||||||||||||||||||||
| Journal or Publication Title: | Monthly Notices of the Royal Astronomical Society | |||||||||||||||||||||||||||
| Publisher: | Oxford University Press | |||||||||||||||||||||||||||
| ISSN: | 0035-8711 | |||||||||||||||||||||||||||
| Official Date: | February 2021 | |||||||||||||||||||||||||||
| Dates: |
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| Volume: | 500 | |||||||||||||||||||||||||||
| Number: | 4 | |||||||||||||||||||||||||||
| Page Range: | pp. 4878-4900 | |||||||||||||||||||||||||||
| DOI: | 10.1093/mnras/staa3335 | |||||||||||||||||||||||||||
| Status: | Peer Reviewed | |||||||||||||||||||||||||||
| Publication Status: | Published | |||||||||||||||||||||||||||
| Publisher Statement: | This is a pre-copyedited, author-produced version of an article accepted for publication in Monthly Notices of the Royal Astronomical Society following peer review. The version of record J B Lovell, M C Wyatt, M Ansdell, M Kama, G M Kennedy, C F Manara, S Marino, L Matrà, G Rosotti, M Tazzari, L Testi, J P Williams, ALMA Survey of Lupus Class III Stars: Early Planetesimal Belt Formation and Rapid Disk Dispersal, Monthly Notices of the Royal Astronomical Society, , staa3335[insert complete citation information here] is available online at: http://dx.doi.org/10.1093/mnras/staa3335 | |||||||||||||||||||||||||||
| Access rights to Published version: | Restricted or Subscription Access | |||||||||||||||||||||||||||
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