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The Atmospheric Variations of the Peculiar B[e] Star HD 45677 (FS CMa)

Published online by Cambridge University Press:  12 April 2016

G. Israelian ,
M. Friedjung ,
J. Graham ,
G. Muratorio ,
C. Rossi  and
D. de Winter
G. Israelian
Affiliation:
Astronomy Group, Vrije Universiteit Brussel, Pleinlaan 2, B-1050 Brussel, Belgium
M. Friedjung
Affiliation:
Institute d’Astrophysique, CNRS, 98bis Bvd. Arago, 75014 Paris, France
J. Graham
Affiliation:
Carnegie Institution of Washington, Dep. of Terrestrial Magnetism, 5241 Broad Branch Road, N.W., Washington, D.C. 20015, USA
G. Muratorio
Affiliation:
Observatoire de Marseille, 2, Place Le Verrier, Marseille, France
C. Rossi
Affiliation:
Instituto Astronomico, Universita La Sapienza, Via Lancisi 29, 00161 Roma, Italy
D. de Winter
Affiliation:
Astronomical Institute “Anton Pannekoek”, University of Amsterdam, Kruislaan 403, 1098 SJ Amsterdam, The Netherlands

Abstract

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We have studied spectra of the peculiar B[e] star HD 45677. Examination of the Balmer wings enabled us to determine a value of log g = 3.9 indicating a possibly luminosity class V. The weak Heɪ lines togetherwith the Si ɪɪ 4128 and 4130 Å doublet indicate a low rotation velocity in the order of 70 km s−1, which is much lower than the previously claimed value of 200 km s−1 by Swings & Allen (1971). We have examined high-resolution profiles of the strong He I line at 5876 Å and found on one hand that we can explain the variation of the profile by the motions of clouds, some of which accreted. The Balmer lines on the other hand show the presence of an accelerated wind plus absorption by a disk seen edge-on

Type
Part 15. Poster Papers
Information
International Astronomical Union Colloquium , Volume 163: Accretion Phenomena and Related Outflows , 1997 , pp. 729
Copyright
Copyright © Astronomical Society of the Pacific 1997

References

Swings, J.P., & Allen, D.A. 1971, ApJ, 167, L41 Google Scholar