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Probing the internal rotation of pre-white dwarf stars with asteroseismology: the case of PG 0122+200

Authors

  • A. H. Córsico,

    Corresponding author
    1. Facultad de Ciencias Astronómicas y Geofísicas, Universidad Nacional de La Plata, Paseo del Bosque s/n, (1900) La Plata, Argentina
    2. Instituto de Astrofísica La Plata (IALP-CONICET), Argentina
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  • L. G. Althaus,

    1. Facultad de Ciencias Astronómicas y Geofísicas, Universidad Nacional de La Plata, Paseo del Bosque s/n, (1900) La Plata, Argentina
    2. Instituto de Astrofísica La Plata (IALP-CONICET), Argentina
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  • S. D. Kawaler,

    1. Department of Physics and Astronomy, Iowa State University, 12 Physics Hall, Ames, IA 50011, USA
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  • M. M. Miller Bertolami,

    1. Facultad de Ciencias Astronómicas y Geofísicas, Universidad Nacional de La Plata, Paseo del Bosque s/n, (1900) La Plata, Argentina
    2. Instituto de Astrofísica La Plata (IALP-CONICET), Argentina
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  • E. García-Berro,

    1. Departament de Física Aplicada, Universitat Politècnica de Catalunya, c/Esteve Terrades 5, 08860 Castelldefels, Spain
    2. Institute for Space Studies of Catalonia, c/Gran Capità 2–4, Edif. Nexus 104, 08034 Barcelona, Spain
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  • S. O. Kepler

    1. Departamento de Astronomia, Universidade Federal do Rio Grande do Sul, Av. Bento Goncalves 9500 Porto Alegre 91501-970, RS, Brazil
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E-mail: acorsico@fcaglp.unlp.edu.ar

ABSTRACT

We put asteroseismological constraints on the internal rotation profile of the GW Vir (PG1159-type) star PG 0122+200. To this end we employ a state-of-the-art asteroseismological model for this star and assess the expected frequency splittings induced by rotation adopting a forward approach in which we compare the theoretical frequency separations with the observed ones assuming different types of plausible internal rotation profiles. We also employ two asteroseismological inversion methods for the inversion of the rotation profile of PG 0122+200. We find evidence for differential rotation in this star. We demonstrate that the frequency splittings of the rotational multiplets exhibited by PG 0122+200 are compatible with a rotation profile in which the central regions are spinning about 2.4 times faster than the stellar surface.

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