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Solar-like oscillation amplitudes and line-widths as a probe for turbulent convection in stars

Published online by Cambridge University Press:  01 August 2006

R. Samadi ,
K. Belkacem ,
M.-J. Goupil ,
F. Kupka  and
M.-A. Dupret
R. Samadi
Affiliation:
Observatoire de Paris, LESIA, Meudon, France; email: reza.samadi@obspm.fr
K. Belkacem
Affiliation:
Observatoire de Paris, LESIA, Meudon, France; email: reza.samadi@obspm.fr
M.-J. Goupil
Affiliation:
Observatoire de Paris, LESIA, Meudon, France; email: reza.samadi@obspm.fr
F. Kupka
Affiliation:
Max-Planck-Institute for Astrophysics, Garching, Germany.
M.-A. Dupret
Affiliation:
Observatoire de Paris, LESIA, Meudon, France; email: reza.samadi@obspm.fr
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Abstract

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Excitation of solar-like oscillations is attributed to turbulent convection and takes place at the upper-most part of the outer convective zones. Amplitudes of these oscillations depend on the efficiency of the excitation processes as well as on the properties of turbulent convection. We present past and recent improvements on the modeling of those processes. We show how the mode amplitudes and mode line-widths can bring information about the turbulence in the specific cases of the Sun and α Cen A.

Keywords

TurbulenceconvectionSun: oscillationsstars: oscillations (including pulsations)stars: Alpha Cen A

Information

Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 2 , Symposium S239: Convection in Astrophysics , August 2006 , pp. 349 - 357
Copyright
Copyright © International Astronomical Union 2007

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