Seismology of delta Scuti stars - GX Pegasi

Details Seismology of delta Scuti stars - GX Pegasi Seismology of delta Scuti stars - GX Pegasi

Feb 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993a%26a...268..546g&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 268, no. 2, p. 546-560.

Statistics

Computation

30

Seismology, Starquakes, Stellar Oscillations, Variable Stars, Charge Coupled Devices, Computational Astrophysics, Hertzsprung-Russell Diagram, Stellar Evolution, Stellar Models, Stellar Rotation

Scientific paper

An identification of the five observed frequencies of the Delta Scuti star GX Pegasi is proposed. It involves two radial modes of radial order n = 2,3 and one nonradial mode 1 = 1, n = 3 split by rotation. It is found that the nonradial mode is mainly trapped in the envelope. The asymmetric pattern of the nonradial mode split by rotation is found quantitatively consistent with departure from symmetry due to second-order effects of rotation and binarity. GX Pegasi belongs to a short period binary system for which synchronization has certainly already taken place. The value of the splitting shows, however, that the star cannot rotate as a solid body and is thus not synchronized down to the core. This ought to provide a constraint on synchronization time scale. A rotational frequency radial profile is assumed which provides an estimation of the central rotational frequency, Omega(c). If only the very outer layers have had time to synchronized, Omega(c) is about 10-13 microHz. The deeper the synchronization has taken place, the larger Omega(c). An independent upper limit on Omega(c) can however be set, which shows that the star cannot be synchronized over more than 70 percent by radius from surface, if overshooting of the convective is to be taken into account.

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