Protoplanetary disk lifetimes vs stellar mass and possible implications for giant planet populations
By 'Alvaro Ribas, H. Bouy, B. Mer'in. 2015
193 citations recorded by the source corpus.
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. We update the protoplanetary disk fractions presented in our recent work (paper I of this series) derived for 22 nearby ( 2 M$_{\odot}$) stars. We also find a roughly constant level of evolved disks throughout the whole age and stellar mass spectra. 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.
Subfields: Astronomy and Astrophysics
View Paper: https://www.semanticscholar.org/paper/eef65cfe9567793df60b23f479619bce75205237
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In Astronomy and Astrophysics
Citations in the corpus
- Evidence for the formation of comet 67P/Churyumov-Gerasimenko through gravitational collapse of a bound clump of pebbles (2017, background): “The disc lifetime is a few million years (Ribas et al. 2015) so that such a delayed planetesimal formation would also help to prevent the planetesimals from melting by short-lifetime radioactive decay (Davidsson et al. 2016).”
- The star formation history and accretion-disc fraction among the K-type members of the Scorpius–Centaurus OB association (2016, unknown): “Ribas et al. (2015) have summarized these mass-dependent disk fraction trends using the nearby young stellar associations within ∼500 pc, and have come to a similar conclusion – that the disk dispersal time depends on stellar mass, with the low-mass stars retaining their disks longer.”
- YOUNG STELLAR OBJECTS IN THE GOULD BELT (2015, methodology): “Very recent results by Ribas et al. (2014) and Ribas et al. (2015), using spectroscopically confirmed members of various young clusters, show that this duration depends on the wavelength where the infrared excess indicative of the presence of a disk first appears, ranging from 1.9 Myr for λ < 5 µm…”