Journal
ASTRONOMY & ASTROPHYSICS
Volume 591, Issue -, Pages -Publisher
EDP SCIENCES S A
DOI: 10.1051/0004-6361/201628549
Keywords
accretion, accretion disks; protoplanetary disks; stars: pre-main sequence; stars: variables: T Tauri, Herbig Ae/Be
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Funding
- ESA Research Fellowship
- DISCSIM project - European Research Council [341137, ERC-2013-ADG]
- Science Foundation Ireland [13/ERC/I2907]
- European Union A-ERC grant [291141 CHEMPLAN]
- Netherlands Research School for Astronomy (NOVA)
- Netherlands Organization for Scientific Research (NWO) [614.001.352]
- NSF
- NASA [AST-1208911, NNX15AC92G]
- Division Of Astronomical Sciences
- Direct For Mathematical & Physical Scien [1208911] Funding Source: National Science Foundation
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A relation between the mass accretion rate onto the central young star and the mass of the surrounding protoplanetary disk has long been theoretically predicted and observationally sought. For the first time, we have accurately and homogeneously determined the photospheric parameters, mass accretion rate, and disk mass for an essentially complete sample of young stars with disks in the Lupus clouds. Our work combines the results of surveys conducted with VLT/X-Shooter and ALMA. With this dataset we are able to test a basic prediction of viscous accretion theory, the existence of a linear relation between the mass accretion rate onto the central star and the total disk mass. We find a correlation between the mass accretion rate and the disk dust mass, with a ratio that is roughly consistent with the expected viscous timescale when assuming an interstellar medium gas-to-dust ratio. This confirms that mass accretion rates are related to the properties of the outer disk. We find no correlation between mass accretion rates and the disk mass measured by CO isotopologues emission lines, possibly owing to the small number of measured disk gas masses. This suggests that the mm-sized dust mass better traces the total disk mass and that masses derived from CO may be underestimated, at least in some cases.
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