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Variable UV Line Emission in S Carinae: Miras Do Not Fear Change

Published online by Cambridge University Press:  15 February 2018

E.W. Brugel ,
R. Davis  and
J. Bookbinder
E.W. Brugel
Affiliation:
CASA, University of Colorado, Boulder, CO
R. Davis
Affiliation:
CASA, University of Colorado, Boulder, CO
J. Bookbinder
Affiliation:
SAO, Cambridge, MA

Abstract

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The object S Carinae is a bright, relatively hot, short (149d) period mira. As expected, the Mg II h and k lines dominate the ultraviolet line spectra during a large fraction of the pulsation cycle. There are also numerous emission lines of Fe I and Fe II produced by either fluorescense or possibly collisional excitation. The unifying “theme” for all the ultraviolet line emission is variability - during a pulsation cycle one observes changes in the intensity, the central wavelength and (for the stronger lines) the line profile.

Type
Beyond the Classical Instability Strip
Information
International Astronomical Union Colloquium , Volume 139: New Perspectives on Stellar Pulsation and Pulsating Variable Stars , 1993 , pp. 210 - 211
Copyright
Copyright © Cambridge University Press 1993

References

Bookbinder, J., Brugel, E.W. and Brown, A., 1989 Astroph. J., 342, 516.Google Scholar
Carpenter, K.G., Pesce, J.E., Stencel, J.E., Brown, A., and Wing, R.F. 1988 Astroph. J. Supp., 68, 345.CrossRefGoogle Scholar