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Be Envelope Properties Determined from Fe II Emission Lines1

Published online by Cambridge University Press:  12 April 2016

J. Chauville ,
D. Ballereau ,
L. Cidale ,
N. Morrell ,
M. Friedjung  and
J. Zorec
J. Chauville
Affiliation:
Observatoire de Paris-Meudon, DASGAL/UMR8633 du CNRS, F-92195 Meudon Principal Cedex, France
D. Ballereau
Affiliation:
Observatoire de Paris-Meudon, DASGAL/UMR8633 du CNRS, F-92195 Meudon Principal Cedex, France
L. Cidale
Affiliation:
Observatorio Astronómico de La Plata, Paseo del bosque S/N, 1900 La Plata, Argentina
N. Morrell
Affiliation:
Observatorio Astronómico de La Plata, Paseo del bosque S/N, 1900 La Plata, Argentina
M. Friedjung
Affiliation:
Institut d’Astrophysique de Paris, CNRS, 98bisBd. Arago, F-75014 Paris, France
J. Zorec
Affiliation:
Institut d’Astrophysique de Paris, CNRS, 98bisBd. Arago, F-75014 Paris, France

Abstract

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Applying the SAC (self absorption curve) method to χ Oph (HD 148184) we conclude that Fell emission lines are optically thick. We estimate the excitation temperature of the permitted Fe II line formation region and the dimensions of this region. We conclude that this region may possibly have a non-uniform density structure.

Type
6. Disks
Information
International Astronomical Union Colloquium , Volume 175: The Be Phenomenon in Early-Type Stars , 2000 , pp. 523 - 526
Copyright
Copyright © Astronomical Society of the Pacific 2000

Footnotes

1

Data obtained in CASLEO operated under agreement between the CONICET and the Universities of La Plata, Córdoba and San Juan - Argentina

References

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Moujtahid, A., Zorec, J., Hubert, A.M. 2000, this volume: “On the characteristics of the CE near the central object”Google Scholar
Muratorio, G., & Friedjung, M. 1988, A&A 190, 103 Google Scholar
Muratorio, G., Viotti, R., Friedjung, M., Baratta, G.B., Rossi, C. 1992, A&A 258, 423 Google Scholar