# The two hybrid B-type pulsators: ν Eridani and 12 Lacertae

@article{Dziembowski2008TheTH,
title={The two hybrid B-type pulsators: $\nu$ Eridani and 12 Lacertae},
author={Wojciech A. Dziembowski and Alexey A. Pamyatnykh},
journal={Monthly Notices of the Royal Astronomical Society},
year={2008},
volume={385},
pages={2061-2068}
}
• Published 16 January 2008
• Physics, Geology
• Monthly Notices of the Royal Astronomical Society
The rich oscillation spectra determined for the two stars, ν Eridani and 12 Lacertae, present an interesting challenge to stellar modelling. The stars are hybrid objects showing not only a number of modes at frequencies typical for β Cep stars but also one mode at frequency typical for SPB stars. We construct seismic models of these stars considering uncertainties in opacity and element distribution. We also present estimate of the interior rotation rate and address the matter of mode…
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## References

SHOWING 1-10 OF 27 REFERENCES
Asteroseismology of the β Cephei star ν Eridani: massive exploration of standard and non-standard stellar models to fit the oscillation data
• Physics, Geology
• 2004
We present the results of a detailed seismic modelling of the Cephei star Eridani with the Li‘ ege evolution and pulsation codes. We selected four clearly detected, well-identified and independent
Asteroseismology of the β Cephei star ν Eridani: interpretation and applications of the oscillation spectrum
• Physics, Geology
• 2004
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.
Abundance analysis of prime B-type targets for asteroseismology. I. Nitrogen excess in slowly-rotating beta Cephei stars
• Physics
• 2006
Seismic modelling of the beta Cephei stars promises major advances in our understanding of the physics of early B-type stars on (or close to) the main sequence. However, a precise knowledge of their
Asteroseismology of the β Cephei star ν Eridani – IV. The 2003–2004 multisite photometric campaign and the combined 2002–2004 data
• Physics
• 2005
We report on the second multisite photometric campaign devoted to ν Eridani (ν Eri). The campaign, carried out from 2003 September 11 to 2004 February 16, was very nearly a replica of the first
Updated Opal Opacities
• Physics
• 1996
The reexamination of astrophysical opacities has eliminated gross discrepancies between a variety of observations and theoretical calculations; thus allowing for more detailed tests of stellar
Asteroseismology of HD 129929: Core Overshooting and Nonrigid Rotation
• Physics, Geology
Science
• 2003
High-quality multicolor Geneva photometric data taken over 21 years of the B3Vstar HD 129929 detect six frequencies, among which appear the effects of rotational splitting with a spacing of ∼0.0121 cycles per day, which implies that the star rotates very slowly.
Diffusion of iron‐group elements in the envelopes of HgMn stars
The observed abundance anomalies for iron-group elements in atmospheres of HgMn stars are due to diffusive movements which are driven by radiation-pressure forces and which persist in the stellar
Catalog of Galactic β Cephei Stars
• Physics
• 2005
We present an extensive and up-to-date catalog of Galactic β Cephei stars. This catalog is intended to give a comprehensive overview of observational characteristics of all known β Cephei stars,
Line formation in solar granulation IV. (O I), O I and OH lines and the photospheric O abundance
• Physics
• 2004
The solar photospheric oxygen abundance has been determined from (O I), O I, OH vibration-rotation and OH pure rotation lines by means of a realistic time-dependent, 3D, hydrodynamical model of the
Metallicities of the β Cephei stars from low-resolution ultraviolet spectra
• Physics
• 2005
We derive basic stellar parameters (angular diameters, effective temperatures, metallicities) and interstellar reddening for all β Cephei stars observed during the IUE satellite mission, including