期刊
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
卷 507, 期 1, 页码 818-833出版社
OXFORD UNIV PRESS
DOI: 10.1093/mnras/stab2112
关键词
accretion; accretion discs; planets and satellites: formation; protoplanetary discs
资金
- European Union's Horizon 2020 research and innovation programme under the Marie SklodowskaCurie grant [823823]
- Netherlands Organisation for Scientific Research (NWO) [016.Veni.192.233]
- STFC Ernest Rutherford Fellowship [ST/T003855/1]
- Office of the Vice Chancellor for Research and Graduate Education at the University of Wisconsin-Madison
- Wisconsin Alumni Research Foundation
- NWO [614.001.352]
- Italian Ministry of Education, Universities and Research [CUP C52I13000140001]
- Deutsche Forschungsgemeinschaft (DFG, German Research Foundation) [FOR 2634/1ER685/11-1]
- DFG cluster of excellence ORIGINS
- European Research Council (ERC) via the ERC Synergy Grant ECOGAL [855130]
- STFC [ST/T003855/1] Funding Source: UKRI
The study focuses on the efficiency of dust radial drift in protoplanetary disc evolution models, showing that radial drift leads to faster dust disc shrinkage than observed, indicating that current models overestimate the effect of radial drift.
A key problem in protoplanetary disc evolution is understanding the efficiency of dust radial drift. This process makes the observed dust disc sizes shrink on relatively short time-scales, implying that discs started much larger than what we see now. In this paper, we use an independent constraint, the gas radius (as probed by CO rotational emission), to test disc evolution models. In particular, we consider the ratio between the dust and gas radius, R-CO/R-dust. We model the time evolution of protoplanetary discs under the influence of viscous evolution, grain growth, and radial drift. Then, using the radiative transfer code radmc with approximate chemistry, we compute the dust and gas radii of the models and investigate how R-CO/R-dust evolves. Our main finding is that, for a broad range of values of disc mass, initial radius, and viscosity, R-CO/R-dust becomes large (>5) after only a short time (<1 Myr) due to radial drift. This is at odds with measurements in young star-forming regions such as Lupus, which find much smaller values, implying that dust radial drift is too efficient in these models. Substructures, commonly invoked to stop radial drift in large, bright discs, must then be present, although currently unresolved, in most discs.
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