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Seismic analysis of the massive β Cephei star 15 Canis Majoris

Published online by Cambridge University Press:  23 January 2015

Przemysław Walczak  and
Gerald Handler
Przemysław Walczak
Affiliation:
Nicolaus Copernicus Astronomical Center, Polish Academy of Sciences email: pwalczak@camk.edu.pl
Gerald Handler
Affiliation:
Nicolaus Copernicus Astronomical Center, Polish Academy of Sciences email: pwalczak@camk.edu.pl
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Abstract

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15 Canis Majoris is a quite massive (M ~ 14 M⊙) main sequence pulsator of the β Cephei type. Recent photometric (Handler 2014) and spectroscopic (Saesen & Briquet, priv. comm.) observations confirm four pulsational frequencies and indicate possible additional modes. We calculated models fitting two frequencies identified as radial and dipole modes. Our analysis indicates rather effective overshooting from the convective core as well as a strong dependence of the minimal required overshooting parameter (αov,min) on the metallicity, Z (αov,min ~ -2.5 Z).

When incorporating the non-adiabatic f-parameter (Daszynśka-Daszkiewicz & Walczak 2009), defined as the ratio of the bolometric flux changes to the radial displacement, significant differences between the opacity tables were obtained. The comparison of the models derived with different codes is also interesting. We used two evolutionary codes: Warsaw-New Jersey (Pamyatnykh et al.1998) and MESA (Paxton et al.2011) and some systematic differences were found.

Keywords

stars: individual 15CMastars: variables: β Cepheistars: interiors
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 9 , Issue S307: New windows on massive stars: asteroseismology, interferometry, and spectropolarimetry , June 2014 , pp. 239 - 240
Copyright
Copyright © International Astronomical Union 2015 

References

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