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    The TWA 3 Young Triple System: Orbits, Disks, Evolution

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    Author
    Kellogg, Kendra cc
    Prato, L.
    Torres, G. cc
    Schaefer, G. H.
    Avilez, I.
    Ruíz-Rodríguez, D.
    Wasserman, L. H. cc
    Bonanos, Alceste Z. cc
    Guenther, E. W.
    Neuhäuser, R.
    Levine, S. E. cc
    Bosh, A. S.
    Morzinski, Katie M. cc
    Close, Laird M. cc
    Bailey, Vanessa
    Hinz, Phil
    Males, Jared R. cc
    Show allShow less
    Affiliation
    Univ Arizona, Steward Observ
    Issue Date
    2017-08-03
    Keywords
    binaries: spectroscopic
    binaries: visual
    circumstellar matter
    stars: individual (TWA 3)
    
    Metadata
    Show full item record
    Publisher
    IOP PUBLISHING LTD
    Citation
    The TWA 3 Young Triple System: Orbits, Disks, Evolution 2017, 844 (2):168 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 have characterized the spectroscopic orbit of the TWA 3A binary and provide preliminary families of probable solutions for the TWA 3A visual orbit, as well as for the wide TWA 3A-B orbit. TWA 3 is a hierarchical triple located at 34 pc in the similar to 10 Myr old TW Hya association. The wide component separation is 1."55; the close pair was first identified as a possible binary almost 20 years ago. We initially identified the 35-day period orbital solution using high-resolution infrared spectroscopy that angularly resolved the A and B components. We then refined the preliminary orbit by combining the infrared data with a reanalysis of our high-resolution optical spectroscopy. The orbital period from the combined spectroscopic solution is similar to 35 days, the eccentricity is similar to 0.63, and the mass ratio is similar to 0.84; although this high mass ratio would suggest that optical spectroscopy alone should be sufficient to identify the orbital solution, the presence of the tertiary B component likely introduced confusion in the blended optical spectra. Using millimeter imaging from the literature, we also estimate the inclinations of the stellar orbital planes with respect to the TWA 3A circumbinary disk inclination and find that all three planes are likely misaligned by at least similar to 30 degrees. The TWA 3A spectroscopic binary components have spectral types of M4.0 and M4.5; TWA 3B is an M3. We speculate that the system formed as a triple, is bound, and that its properties were shaped by dynamical interactions between the inclined orbits and disk.
    ISSN
    1538-4357
    DOI
    10.3847/1538-4357/aa7c60
    Version
    Final published version
    Sponsors
    NSF [AST-1009136, AST-1313399, AST-1509375, AST-1411654]; NASA Space Grant, through Northern Arizona University; NASA Exoplanets Research Program (XRP) [NNX16AD44G]; National Science Foundation [AST-1005313]; National Aeronautics and Space Administration; National Science Foundation; W. M. Keck Foundation
    Additional Links
    http://stacks.iop.org/0004-637X/844/i=2/a=168?key=crossref.570a8b969db9ac6657b634e76178b9a7
    ae974a485f413a2113503eed53cd6c53
    10.3847/1538-4357/aa7c60
    Scopus Count
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    UA Faculty Publications

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