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    High-velocity Bullets from V Hydrae, an Asymptotic Giant Branch Star in Transition: Ejection History and Spatio-kinematic Modeling

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    Scibelli_2019_ApJ_870_117.pdf
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    Description:
    Final Published version
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    Author
    Scibelli, S.
    Sahai, R.
    Morris, M. R.
    Affiliation
    Univ Arizona, Steward Observ
    Issue Date
    2019-01-10
    Keywords
    circumstellar matter
    stars: AGB and post-AGB
    stars: jets
    stars: individual (V Hydrae)
    stars: mass-loss
    
    Metadata
    Show full item record
    Publisher
    IOP PUBLISHING LTD
    Citation
    S. Scibelli et al 2019 ApJ 870 117
    Journal
    ASTROPHYSICAL JOURNAL
    Rights
    © 2019. 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
    The carbon star V Hydrae (V Hya) provides new insight into the nature of the launching mechanism of jet-like outflows that are believed to be the cause of the poorly understood transition phase of asymptotic giant branch stars into aspherical planetary nebulae. V Hya has been shown to periodically eject collimated gas blobs at high velocities ("bullets"). By analyzing data from Hubble Space Telescope/Space Telescope Imaging Spectrograph 2D spectra, obtained at six epochs spaced over a decade that show four successively ejected bullets with a spacing of 8.5 yr, we have created kinematic models of the dynamical evolution of a specific bullet (#1) for the first three observed epochs (2002, 2003, 2004) using a 3D spatio-kinematic code, SHAPE. Using these models, we fit the observed morphology, line-of-sight velocity, proper motion, and intensity for the extended, gaseous bullet as a function of time over a period of 2 yr, in order to constrain its 3D movement and the evolution of its physical properties over this period. Our results suggest that although bullet #1's motion is predominantly ballistic, there are small but significant changes in the position angle and inclination angle of the long (symmetry) axis of the bullet that tilt it progressively toward the symmetry axis of the bipolar molecular nebula around V Hya. In contrast, bullet #3 shows strong acceleration soon after ejection. We discuss the possibilities that bullet acceleration is caused by a nonradial magnetic field and/or by hydrodynamic interaction with the ambient gas through which the bullet is traveling.
    ISSN
    1538-4357
    DOI
    10.3847/1538-4357/aaf21b
    Version
    Final published version
    Sponsors
    STScI HST award [GO 12227.01]; NASA
    Additional Links
    http://stacks.iop.org/0004-637X/870/i=2/a=117?key=crossref.53b721a880e54c281c55fde506a31bfe
    ae974a485f413a2113503eed53cd6c53
    10.3847/1538-4357/aaf21b
    Scopus Count
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    UA Faculty Publications

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