Asteroseismology of the β Cephei star ν Eridani: interpretation and applications of the oscillation spectrum

By A. Pamyatnykh, G. Handler, W. Dziembowski. 2004

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The oscillation spectrum of v Eri is the richest known for any variable of the β Cephei type. We interpret the spectrum in terms of normal mode excitation and construct seismic models of the star. The frequency data combined with data on mean colours set the upper limit on the extent of overshooting from the convective core. We use data on rotational splitting of two dipole (l = 1) modes (g 1 and p 1 ) to infer properties of the internal rotation rate. Adopting a plausible hypothesis of nearly uniform rotation in the envelope and increasing rotation rate in the μ-gradient zone, we find that the mean rotation rate in this zone is about three times faster than in the envelope. In our standard model only the modes in the middle part of the oscillation spectrum are unstable. To account for excitation of a possible high-order g mode at v = 0.43 cd -1 as well as p modes at v > 6 cd -1 we have to invoke an overabundance of Fe in the driving zone.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/956a7ea37ee3812bcca46f4507cac592479da6e6

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MODULES FOR EXPERIMENTS IN STELLAR ASTROPHYSICS (MESA) (2010, background): “:3) star from Pamyatnykh et al. (2004).”
Catalog of Galactic β Cephei Stars (2005, background): “A recentmultisite,multitechnique campaign for another Cephei star, Eridani (Handler et al. 2004; Aerts et al. 2004a) enabled seismicmodeling aswell (Pamyatnykh et al. 2004; Ausseloos et al. 2004).”
Massive pulsating stars observed by BRITE-Constellation - I. The triple system β Centauri (Agena) (2016, background): “This indicates a possible need for revision of the opacities, see Pamyatnykh et al. (2004), Miglio et al. (2007), Zdravkov & Pamyatnykh (2008), and Walczak et al. (2013, 2015).”