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    M STARS IN THE TW HYA ASSOCIATION: STELLAR X-RAYS AND DISK DISSIPATION

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    Kastner_2016_AJ_152_3.pdf
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    Author
    Kastner, Joel H. cc
    Principe, David A. cc
    Punzi, Kristina cc
    Stelzer, Beate cc
    Gorti, Uma cc
    Pascucci, Ilaria cc
    Argiroffi, Costanza
    Affiliation
    Univ Arizona, Lunar & Planetary Lab
    Issue Date
    2016-06-13
    Keywords
    circumstellar matter
    planets and satellites: formation
    stars: formation
    stars: pre-main sequence
    
    Metadata
    Show full item record
    Publisher
    IOP PUBLISHING LTD
    Citation
    M STARS IN THE TW HYA ASSOCIATION: STELLAR X-RAYS AND DISK DISSIPATION 2016, 152 (1):3 The Astronomical Journal
    Journal
    The Astronomical Journal
    Rights
    © 2016. 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
    To investigate the potential connection between the intense X-ray emission from young low-mass stars and the lifetimes of their circumstellar planet-forming disks, we have compiled the X-ray luminosities (L-X) of M stars in the similar to 8 Myr old TW Hya Association (TWA) for which X-ray data are presently available. Our investigation includes analysis of archival Chandra data for the TWA binary systems TWA 8, 9, and 13. Although our study suffers from poor statistics for stars later than M3, we find a trend of decreasing L-X/L-bol with decreasing T-eff for TWA M stars, wherein the earliest-type (M0-M2) stars cluster near log(L-X/L-bol) approximate to -3.0 and then log(L-X/L-bol) decreases, and its distribution broadens, for types M4 and later. The fraction of TWA stars that display evidence for residual primordial disk material also sharply increases in this same (mid-M) spectral type regime. This apparent anticorrelation between the relative X-ray luminosities of low-mass TWA stars and the longevities of their circumstellar disks suggests that primordial disks orbiting early-type M stars in the TWA have dispersed rapidly as a consequence of their persistent large X-ray fluxes. Conversely, the disks orbiting the very lowest-mass pre-MS stars and pre-MS brown dwarfs in the Association may have survived because their X-ray luminosities and, hence, disk photoevaporation rates are very low to begin with, and then further decline relatively early in their pre-MS evolution.
    ISSN
    1538-3881
    DOI
    10.3847/0004-6256/152/1/3
    Version
    Final published version
    Sponsors
    NASA Astrophysics Data Analysis Program [NNX12AH37G]; NASA Exoplanets program [NNX16AB43G]; National Science Foundation [AST-1108950]; CONICYT-FONDECYT [3150550]; Millennium Science Initiative (Chilean Ministry of Economy) [RC 130007]
    Additional Links
    http://stacks.iop.org/1538-3881/152/i=1/a=3?key=crossref.7e1b04a4b49e1c69f2d1d6677336d7bd
    ae974a485f413a2113503eed53cd6c53
    10.3847/0004-6256/152/1/3
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    UA Faculty Publications

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