Journal
ASTRONOMY & ASTROPHYSICS
Volume 576, Issue -, Pages -Publisher
EDP SCIENCES S A
DOI: 10.1051/0004-6361/201424846
Keywords
protoplanetary disks; planet-disk interactions; stars: formation; planetary systems; stars: pre-main sequence
Categories
Funding
- ESAC Science Operations Division [SC 1300016149]
- ESAC Space Science Faculty
- Herschel Science Centre
- Spanish Ramon y Cajal fellowship [RYC-2009-04497]
- Alfred P. Sloan Foundation
- National Science Foundation
- US Department of Energy Office of Science
- University of Arizona
- Brazilian Participation Group
- Brookhaven National Laboratory
- University of Cambridge
- University of Florida
- French Participation Group
- German Participation Group
- Instituto de Astrofisica de Canarias
- Michigan State/Notre Dame/JINA Participation Group
- Johns Hopkins University
- Lawrence Berkeley National Laboratory
- Max Planck Institute for Astrophysics
- New Mexico State University
- New York University
- Ohio State University
- Pennsylvania State University
- University of Portsmouth
- Princeton University
- Spanish Participation Group
- University of Tokyo
- University of Utah
- Vanderbilt University
- University of Virginia
- University of Washington
- Yale University
- French Institut National des Sciences de l'Univers
- CNRS
- French Education Ministry
- European Southern Observatory
- State of Baden-Wuerttemberg
- European Commission under networks of the SCIENCE and Human Capital and Mobility programs
- Landessternwarte
- Heidelberg
- Institut d'Astrophysique de Paris
- National Aeronautics and Space Administration
- NASA
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Aims. We study the dependence of protoplanetary disk evolution on stellar mass using a large sample of young stellar objects in nearby young star-forming regions. Methods. We update the protoplanetary disk fractions presented in our recent work (Paper I of this series) derived for 22 nearby (<500 pc) associations between 1 and 100 Myr. We use a subsample of 1428 spectroscopically confirmed members to study the impact of stellar mass on protoplanetary disk evolution. We divide this sample into two stellar mass bins (2 M-circle dot boundary) and two age bins (3 Myr boundary), and use infrared excesses over the photospheric emission to classify objects in three groups: protoplanetary disks, evolved disks, and diskless. The homogeneous analysis and bias corrections allow for a statistically significant inter-comparison of the obtained results. Results. We find robust statistical evidence of disk evolution dependence with stellar mass. Our results, combined with previous studies on disk evolution, confirm that protoplanetary disks evolve faster and/or earlier around high-mass (>2 M-circle dot) stars. We also find a roughly constant level of evolved disks throughout the whole age and stellar mass spectra. Conclusions. We conclude that protoplanetary disk evolution depends on stellar mass. Such a dependence could have important implications for gas giant planet formation and migration, and could contribute to explaining the apparent paucity of hot Jupiters around high-mass stars.
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