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Seismology of δ Scuti Stars: Problems and Prospects

Published online by Cambridge University Press:  12 April 2016

M.J. Goupil  and
S. Talon
M.J. Goupil
Affiliation:
Observatoire de Paris, DASGAL, URA 335, Paris, France, mariejo.goupil@obspm.fr
S. Talon
Affiliation:
CERCA and Dépt. de Physique, Université de Montréal, Québec, talon@cerca.umontreal.ca

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The current state of seismology of δ Scuti stars is reviewed with particular emphasis on seismic signatures of the extension of their mixed central region and of rotation. We refer also to Goupil et al. (2000) and more generally to Breger & Montgomery (2000) for more details.

δ Scuti stars are population I pulsating stars with spectral type A-early F, located on or near the main sequence. They are found in the lower part of the classical instability strip in a HR diagram (Fig. 1). Masses range from ∼ 1.5M⊙ to ∼ 2.5M⊙ and δ Scuti stars are either in a stage of H-core or H-shell burning. On the main sequence, the high temperature sensitivity of the dominant CNO cycle causes a large convective core to develop, which later shrinks leaving behind a gradient ∇μ in the mean molecular weight.

Type
Part 2.4. Delta Scuti Stars
Information
International Astronomical Union Colloquium , Volume 185: Radial and Nonradial Pulsations as Probes of Stellar Physics , 2002 , pp. 306 - 318
Copyright
Copyright © Astronomical Society of the Pacific 2002

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