Volume 465, Number 3, April III 2007
|Page(s)||937 - 942|
|Section||Stellar structure and evolution|
|Published online||05 February 2007|
Nonradial oscillations in classical Cepheids: the problem revisited
CRAL, CNRS, UMR 5574, École normale supérieure, 46 allée d'Italie, 69007 Lyon, France e-mail: [cedric.mulet-marquis;ibaraffe;cwinisdo]@ens-lyon.fr
2 Institut für Astrophysik, Georg-August-Universität Göttingen, Friedrich-Hund-Platz 1, 37077 Göttingen, Germany e-mail: email@example.com
Accepted: 2 January 2007
Context.We analyse the presence of nonradial oscillations in Cepheids, a problem that has not been theoretically revised since the work of Dziembowski (1977, Acta Astron., 27, 95) and Osaki (1977, PASJ, 29, 235). Our analysis is motivated by a work of Moskalik et al. (2004, ASPC, 310, 498), which reports the detection of low-amplitude periodicities in a few Cepheids of the large Magellanic cloud. These newly discovered periodicities were interpreted as nonradial modes.
Aims.Based on linear nonadiabatic stability analysis, our goal is to reanalyse the presence and stability of nonradial modes, taking into account improvement in the main input physics required for the modelling of Cepheids.
Methods.We compare the results obtained from two different numerical methods used to solve the set of differential equations: a matrix method and the Ricatti method.
Results.We show the limitation of the matrix method for finding low-order p-modes (), because of their dual character in evolved stars such as Cepheids. For higher order p-modes, we find excellent agreement between the two methods.
Conclusions.No nonradial instability is found below , whereas many unstable nonradial modes exist for higher orders. We also find that nonradial modes remain unstable, even at hotter effective temperatures than the blue edge of the Cepheid instability strip, where no radial pulsations are expected.
Key words: stars: oscillations
© ESO, 2007
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