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    New observations and asteroseismic analysis of the subdwarf B pulsator PG 1219+534

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    Author
    Van Grootel, Valérie
    Péters, Marie-Julie
    Green, Elizabeth M.
    Charpinet, Stéphane
    Brassard, Pierre
    Fontaine, Gilles
    Affiliation
    Univ Arizona, Steward Observ
    Issue Date
    2018-02
    Keywords
    subdwarfs
    stars: oscillation
    stars:interior
    stars: individual: PG 1219+534
    
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    Publisher
    DE GRUYTER POLAND SP ZOO
    Citation
    Open Astronomy, Volume 27, Issue 1, Pages 44–56, ISSN (Online) 2543-6376, DOI: https://doi.org/10.1515/astro-2018-0014.
    Journal
    OPEN ASTRONOMY
    Rights
    © 2018, published by De Gruyter. This work is licensed under the Creative Commons Attribution-NonCommercial-NoDerivatives 4.0 License.
    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 present a new asteroseismic modeling of the hot B subdwarf (sdB) pulsator PG 1219+534, based on a 3-month campaign with the Mont4K/Kuiper combination at Mt Bigelow (Arizona) and on updated atmospheric parameters from high S/N low and medium resolution spectroscopy. On the basis of the nine independent pulsation periods extracted from the photometric light curve, we carried out an astroseismic analysis by applying the forward modeling approach using our latest (third and fourth generation) sdB models. Atmospheric parameters (T-eff = 34 258 +/- 170 K, log g = 5.838 +/- 0.030) were used as independent constraints, as well as partial mode identification based on observed multiplet structures we ascribed to stellar rotation. The optimal model found is remarkably consistent between various analyses with third and fourth generation of sdB models, and also with previously published analysis with second generation sdB models. It corresponds to a sdB with a canonical mass (0.46 +/- 0.02 M-circle dot), rather thin H-He envelope (log q(envl) = -3.75 +/- 0.12), and close to He-burning exhaustion (X-core(C + O) = 0.86 +/- 0.05). We also investigate the internal rotation of the star. We find that PG 1219+534 rotates very slowly (P-rot = 34.91 +/- 0.84 days) and that solid-body rotation is reached at least down to similar to 60% of the radius.
    Note
    Open access journal.
    ISSN
    2543-6376
    DOI
    10.1515/astro-2018-0014
    Version
    Final published version
    Additional Links
    http://www.degruyter.com/view/j/astro.2018.27.issue-1/astro-2018-0014/astro-2018-0014.xml
    ae974a485f413a2113503eed53cd6c53
    10.1515/astro-2018-0014
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