Pre-main-sequence isochrones - II. Revising star and planet formation time-scales

By C. Bell, T. Naylor, N. Mayne, R. Jeffries, S. Littlefair. 2013

179 citations recorded by the source corpus.

CPMB is funded by a UK Science and Technology Facilities Council (STFC) studentship. SPL is supported by an RCUK fellowship. The authors would like to thank Charles D. H. Williams for maintaining the Xgrid facilities at the University of Exeter which were used to reduce the photometric data presented in this study. The authors thank Amelia Bayo for bringing to our attention the important work on the λ Ori region published in Bayo et al. (2011) and Bayo et al. (2012) which we overlooked in our original submission. The inclusion of these works does not change the results or conclusions of the paper. The authors also thank the referee for useful comments and constructive suggestions that have greatly improved this work. This research has made use of data obtained at the Isaac Newton Telescope which is operated on the island of La Palma by the Isaac Newton Group (ING) in the Spanish Observatorio del Roque de los Muchachos of the Institutio de Astrofisica de Canarias. This research has also made use of archival data products from the Two-Micron All-Sky Survey (2MASS), which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center, funded by the National Aeronautics and Space Administration (NASA) and the National Science Foundation.

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Citations in the corpus

AN OPTICAL SPECTROSCOPIC STUDY OF T TAURI STARS. I. PHOTOSPHERIC PROPERTIES (2014, background): “These higher extinctions would yield accretion rates of 10−7 M⊙ yr −1, fast enough that steady accretion over the ∼ 2 − 3 Myr CTTS phase would account for ∼ 20 − 50% of the final stellar mass, or more with the older ages measured by Bell et al. (2013).”
Dust Evolution and the Formation of Planetesimals (2016, background): “An improved age estimates of young clusters indicate the disk lifetimes could be much longer (10–12Myr) than we thought before (Bell et al. 2013, see also Pfalzner et al. 2014).”
Magnetic Inhibition of Convection and the Fundamental Properties of Low-Mass Stars. III. A Consistent 10 Myr Age for the Upper Scorpius OB Association (2016, background): “Pre-main-sequence stars typically appear a factor of 2 – 5 younger than main-sequence stars in the same population (Naylor 2009; Bell et al. 2012, 2013).”
YOUNG STELLAR OBJECTS IN THE GOULD BELT (2015, background): “Although the ages of young stars are highly uncertain, recent studies suggest a revised half-life for disk survival of 2.5 − 4 Myr on both observational (e.g., Kraus et al. 2012; Bell et al. 2013; Soderblom et al. 2014) and theoretical (e.g., Alexander & Armitage 2009) grounds.”
Protoplanetary disk lifetimes vs stellar mass and possible implications for giant planet populations (2015, background): “Absolute ages of young associations are hard to determine, and some recent works have shown that the adopted values may be underestimated by a factor of two (Bell et al. 2013).”
Globular clusters as the relics of regular star formation in ‘normal’ high-redshift galaxies (2015, background): “…discs to survive for 5–10Myr (the disc lifetime problem), which may be longer than discs survive in nearby star-forming regions (Haisch, Lada & Lada 2001; Bell et al. 2013), especially at the extreme stellar densities of GCs (Adams et al. 2004; de Juan Ovelar et al. 2012; Rosotti et al. 2014).”
The star formation history and accretion-disc fraction among the K-type members of the Scorpius–Centaurus OB association (2016, background): “This is ∼2 Myr longer than the timescale estimated in Mamajek (2009), and would imply a longer timescale available for planet formation, but consistent with the findings of Bell et al. (2013).”
A self-consistent, absolute isochronal age scale for young moving groups in the solar neighbourhood (2015, methodology): “In a series of papers (Bell et al. 2012, 2013, 2014) we discussed some of the main issues with using pre-main-sequence (pre-MS) model isochrones to derive ages for young clusters in colour-magnitude diagrams (CMDs), and in particular, the inability of these models to reproduce the observed loci in…”
Improved angular momentum evolution model for solar-like stars II. Exploring the mass dependence (2015, unknown): “Observations thus suggest an average disk lifetime of 3 − 5 Myr, and a maximum lifetime of order of 10 − 20 Myr (Bell et al. 2013).”
A lithium depletion boundary age of 21 Myr for the Beta Pictoris moving group (2013, background): “Nevertheless, Jeffries et al. (2013) and Bell et al. (2013) have recently shown that for NGC 1960, a rich open cluster with a similar LDB age to the BPMG, that isochronal fits to both low- and high-mass stars do agree with the LDB age when these problems are carefully considered; the same may yet…”
Separating gas-giant and ice-giant planets by halting pebble accretion (2014, background): “Additionally, the gaseous envelope grows only slowly on Myr timescales, because of the continued heating by accretion of remnant planetesimals, even after clearing most of its feeding zone (Pollack et al. 1996; Ikoma et al. 2000).”