Hostname: page-component-cd9895bd7-8ctnn Total loading time: 0 Render date: 2024-12-26T03:35:15.022Z Has data issue: false hasContentIssue false
  • English
  • Français

IR-radio spectral indices for Be stars

Published online by Cambridge University Press:  26 May 2016

H. Chen ,
A. R. Taylor ,
S.M. Dougherty  and
L.B.F.M. Waters
H. Chen
Affiliation:
University of Calgary, Canada
A. R. Taylor
Affiliation:
University of Calgary, Canada
S.M. Dougherty
Affiliation:
John Moores University of Liverpool, UK
L.B.F.M. Waters
Affiliation:
SRON Laboratory for Space Research, The Netherlands

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

Using published data and new data from mm observations, we calculate spectral indices α(12μ-25μ), α(25μ-1.1mm) and α(1.1mm-2cm) for Be stars. The index α(25μ-1.1mm), obtained for 8 stars, shows two characteristics: 1) for “normal” Be stars the index decreases from earlier types towards later types, i.e., later type Be stars tend to have shallower spectra in the IR-radio region than earlier types; 2) the index for shell stars appears to have smaller values than that for normal Be stars with same spectral types.

Type
6. Be Stars: Circumstellar Environment
Information
Symposium - International Astronomical Union , Volume 162: Pulsation, Rotation and Mass Loss in Early-Type Stars , 1994 , pp. 429 - 430
Copyright
Copyright © Kluwer 1994 

References

The References

Taylor, A.R., Waters, L.B.F.M., Lamers, H.G.L.M., Persi, P., & Bjorkman, K.S., Mon. Not. R. ast. Soc. 288, 811 (1987).Google Scholar
Taylor, A.R., Waters, L.B.F.M., Bjorkman, K.S. & Dougherty, S.M., Astr. Astrophys. 231, 453 (1990). 172, 225 (1987).Google Scholar