Non-adiabatic asteroseismology of near-main sequence variable stars

Details Non-adiabatic asteroseismology of near-main sequence variable stars Non-adiabatic asteroseismology of near-main sequence variable stars

May 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004aspc..310..458d&link_type=abstract

Variable Stars in the Local Group, IAU Colloquium 193, Proceedings of the conference held 6-11 July, 2003 at Christchurch, New Z

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We present in this talk a new linear non-adiabatic pulsation code: MAD1. We detail all the possible applications of it in the frame of asteroseismology. By using it, photospheric observables such as multi-color photometric amplitude ratios, phase differences and line profile variations can be determined accurately and confronted with observations. Moreover, MAD enables the precisely analysis of the excitation mechanisms of pulsating stars. Applications to different kinds of variable stars (δ Sct, β Cephei, Slowly Pulsating B and γ Dor stars) are presented by Dupret et al. (these proceedings), Handler and Aerts (these proceedings), De Cat et al. (these proceedings) and De Ridder et al. (these proceedings).

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