EDP Sciences
The CoRoT space mission: early results
Free Access
Volume 506, Number 1, October IV 2009
The CoRoT space mission: early results
Page(s) 189 - 201
Section Stellar structure and evolution
DOI https://doi.org/10.1051/0004-6361/200811510
Published online 01 April 2009
A&A 506, 189-201 (2009)
DOI: 10.1051/0004-6361/200811510

Pulsation modes in rapidly rotating stellar models based on the self-consistent field method

D. R. Reese1, K. B. MacGregor2, S. Jackson2, A. Skumanich2, and T. S. Metcalfe2

1  Department of Applied Mathematics, University of Sheffield, Hicks Building, Hounsfield Road, S3 7RH, Sheffield, UK
    e-mail: d.reese@sheffield.ac.uk
2  High Altitude Observatory, National Center for Atmospheric Research, Boulder, CO 80307, USA

Received 12 December 2008 / Accepted 23 March 2009

Context. New observational means such as the space missions CoRoT and Kepler and ground-based networks are and will be collecting stellar pulsation data with unprecedented accuracy. A significant fraction of the stars in which pulsations are observed are rotating rapidly.
Aims. Our aim is to characterise pulsation modes in rapidly rotating stellar models so as to be able to interpret asteroseismic data from such stars.
Methods. A new pulsation code is applied to stellar models based on the self-consistent field (SCF) method.
Results. Pulsation modes in SCF models follow a similar behaviour to those in uniformly rotating polytropic models, provided that the rotation profile is not too differential. Pulsation modes fall into different categories, the three main ones being island, chaotic, and whispering gallery modes, which are rotating counterparts to modes with low, medium, and high $\l -\vert m\vert$ values, respectively. The frequencies of the island modes follow an asymptotic pattern quite similar to what was found for polytropic models. Extending this asymptotic formula to higher azimuthal orders reveals more subtle behaviour as a function of m and provides a first estimate of the average advection of pulsation modes by rotation. Further calculations based on a variational principle confirm this estimate and provide rotation kernels that could be used in inversion methods. When the rotation profile becomes highly differential, it becomes more and more difficult to find island and whispering gallery modes at low azimuthal orders. At high azimuthal orders, whispering gallery modes, and in some cases island modes, reappear.
Conclusions. The asymptotic formula found for frequencies of island modes can potentially serve as the basis of a mode identification scheme in rapidly rotating stars when the rotation profile is not too differential.

Key words: stars: oscillations -- stars: rotation

© ESO 2009

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