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    The First 40 Million Years of Circumstellar Disk Evolution: The Signature of Terrestrial Planet Formation

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    Meng_2017_ApJ_836_34.pdf
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    Final Published Version
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    Author
    Meng, Huan Y. A. cc
    Rieke, George H. cc
    Su, Kate Y. L. cc
    Gáspár, András cc
    Affiliation
    Univ Arizona, Dept Astron, Steward Observ
    Univ Arizona, Lunar & Planetary Lab, Dept Planetary Sci
    Issue Date
    2017-02-07
    Keywords
    circumstellar matter
    infrared: planetary systems
    methods: observational
    
    Metadata
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    Publisher
    IOP PUBLISHING LTD
    Citation
    The First 40 Million Years of Circumstellar Disk Evolution: The Signature of Terrestrial Planet Formation 2017, 836 (1):34 The Astrophysical Journal
    Journal
    The Astrophysical Journal
    Rights
    © 2017. The American Astronomical Society. All rights reserved.
    Collection Information
    This item from the UA Faculty Publications collection is made available by the University of Arizona with support from the University of Arizona Libraries. If you have questions, please contact us at repository@u.library.arizona.edu.
    Abstract
    We characterize the first 40 Myr of evolution of circumstellar disks through a unified study of the infrared properties of members of young clusters and associations with ages from 2 Myr up to similar to 40 Myr: NGC 1333, NGC 1960, NGC 2232, NGC 2244, NGC 2362, NGC 2547, IC 348, IC 2395, IC 4665, Chamaeleon I, Orion OB1a and OB1b, Taurus, the beta Pictoris Moving Group,. Ophiuchi, and the associations of Argus, Carina, Columba, Scorpius-Centaurus, and Tucana-Horologium. Our work features: (1) a filtering technique to flag noisy backgrounds; (2) a method based on the probability distribution of deflections, P(D), to obtain statistically valid photometry for faint sources; and (3) use of the evolutionary trend of transitional disks to constrain the overall behavior of bright disks. We find that the fraction of disks three or more times brighter than the stellar photospheres at 24 mu m decays relatively slowly initially and then much more rapidly by similar to 10 Myr. However, there is a continuing component until similar to 35 Myr, probably due primarily to massive clouds of debris generated in giant impacts during the oligarchic/chaotic growth phases of terrestrial planets. If the contribution from primordial disks is excluded, the evolution of the incidence of these oligarchic/chaotic debris disks can be described empirically by a log-normal function with the peak at 12-20 Myr, including similar to 13% of the original population, and with a post-peak mean duration of 10-20 Myr.
    ISSN
    1538-4357
    DOI
    10.3847/1538-4357/836/1/34
    Version
    Final published version
    Sponsors
    National Aeronautics and Space Administration; Caltech/JPL [1255094, 1256424]; NASA [NNX10AD38G]; National Science Foundation
    Additional Links
    http://stacks.iop.org/0004-637X/836/i=1/a=34?key=crossref.bddd0efe2f7dbff5e426af9496a3050a
    ae974a485f413a2113503eed53cd6c53
    10.3847/1538-4357/836/1/34
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    UA Faculty Publications

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