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The (B0+?)+O6 system FN CMa†: a case for tidal-pulsational interaction?

Published online by Cambridge University Press:  12 July 2011

Thomas Rivinius ,
Otmar Stahl ,
Stanislas Štefl ,
Dietrich Baade ,
Richard H.D. Townsend  and
Luis Barrera
Thomas Rivinius
Affiliation:
ESOChile
Otmar Stahl
Affiliation:
LSW/ZAH Heidelberg, Germany
Stanislas Štefl
Affiliation:
ESOChile
Dietrich Baade
Affiliation:
ESOGermany
Richard H.D. Townsend
Affiliation:
UW Madison, USA
Luis Barrera
Affiliation:
UMCE Santiago, Chile
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Abstract

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FN CMa is visually double with a separation of ~0.6 arcsec. Sixty high-cadence VLT/UVES spectra permit the A and B components to be disentangled, as the relative contribution of each star to the total light entering the spectrograph fluctuates between exposures due to changes in seeing. Component A exhibits rapid line-profile variations, leading us to attribute the photometric variability seen by HIPPARCOS (with a derived P = 0.08866 d) to this component. From a total of 122 archival and new echelle spectra it is shown that component A is an SB1 binary with an orbital period of 117.55 days. The eccentricity of 0.6 may result in tidal modulation of the pulsation(s) of component Aa.

Keywords

stars: binaries: generalstars: oscillations (including pulsations)stars: early-type
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 6 , Symposium S272: Active OB stars: structure, evolution, mass loss, and critical limits , July 2010 , pp. 543 - 544
Copyright
Copyright © International Astronomical Union 2011

References

† Based on data from ESO programs 076.C-0431, 076.C-0164, and the BESO spectrograph.