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Deep Photospheric Emission Lines as Probes for Pulsational Waves

Published online by Cambridge University Press:  23 January 2015

Th. Rivinius ,
M. Shultz  and
G. A. Wade
Th. Rivinius
Affiliation:
ESO - European Organisation for Astronomical Research in the Southern Hemisphere, Chile email: [email protected]
M. Shultz
Affiliation:
ESO - European Organisation for Astronomical Research in the Southern Hemisphere, Chile email: [email protected] Dept. of Physics, Engineering Physics and Astronomy, Queen's University, Canada Dept. of Physics, Royal Military College of Canada, Canada
G. A. Wade
Affiliation:
Dept. of Physics, Engineering Physics and Astronomy, Queen's University, Canada Dept. of Physics, Royal Military College of Canada, Canada
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Abstract

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Weak line emission originating in the photosphere is well known from O stars and widely used for luminosity classification. The physical origin of the line emission are NLTE effects, most often optical pumping by far-UV lines. Analogous lines in B stars of lower luminosity are identified in radially pulsating β Cephei stars. Their diagnostic value is shown for radially pulsating stars, as these lines probe a much larger range of the photosphere than absorption lines, and can be traced to regions where the pulsation amplitude is much lower than seen in the absorption lines.

Keywords

stars: oscillationsstars: atmospheresstars: individual (ξ1 CMa, BW Vul)
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. 228 - 229
Copyright
Copyright © International Astronomical Union 2015 

References

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