Hostname: page-component-cc8bf7c57-n7qbj Total loading time: 0 Render date: 2024-12-12T06:29:35.887Z Has data issue: false hasContentIssue false
  • English
  • Français

The dust composition of discs surrounding isolated Herbig Ae/Be stars

Published online by Cambridge University Press:  26 May 2016

G. Meeus ,
J. Bouwman ,
L.B.F.M. Waters ,
C. Waelkens  and
M.E. van den Ancker
G. Meeus
Affiliation:
Astronomical Institute, K. U. Leuven, Celestijnenlaan 200B, B-3001 Leuven, Belgium
J. Bouwman
Affiliation:
Astronomical Institute “Anton Pannekoek”, University of Amsterdam, Kruislaan 403, NL-1098 SJ Amsterdam, The Netherlands
L.B.F.M. Waters
Affiliation:
Astronomical Institute “Anton Pannekoek”, University of Amsterdam, Kruislaan 403, NL-1098 SJ Amsterdam, The Netherlands
C. Waelkens
Affiliation:
Astronomical Institute, K. U. Leuven, Celestijnenlaan 200B, B-3001 Leuven, Belgium
M.E. van den Ancker
Affiliation:
Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, MS 42, Cambridge, MA 02138, USA

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.

We present Infrared Space Observatory (ISO) spectra of 14 isolated Herbig Ae/Be stars. The IR spectra were combined with photometric data from the UV to the sub-mm region. We defined two key groups, based upon the spectral shape of the IR region. The results can be summarized as follows (see also Meeus et al. 2001): (1) the continuum of the IR to sub-mm region can be reconstructed by the sum of a power-law and a cool component, which can be represented by a black body. Possible locations for these components are an optically thick, geometrically thin disc (power-law component) and an optically thin flared region (black body); (2) remarkably, some sources lack the silicate bands; (3) PAH bands are present in at least 50% of our sample; with one exception, PAHs are not present in sources which only show a power-law continuum in the IR; (4) the dust in HAEBE stars shows strong evidence for coagulation; this dust processing is unrelated to any of the central star properties.

Type
Part IV: Protoplanetary and β Pic disks
Information
Symposium - International Astronomical Union , Volume 202: Planetary Systems in the Universe – Observation, Formation and Evolution , 2004 , pp. 356 - 358
Copyright
Copyright © Astronomical Society of the Pacific 2004 

References

Chiang, E.I., & Goldreich, P. 1997, ApJ, 490, 368.CrossRefGoogle Scholar
de Graauw, M.S., Haser, L.N., Beintema, M.A. et al. 1996, A&A, 315, L49.Google Scholar
Herbig, G.H. 1960, ApJS, 4, 337.CrossRefGoogle Scholar
Kenyon, S.J., & Hartmann, L. 1987, ApJ, 323, 714.CrossRefGoogle Scholar
Meeus, G., Waters, L.B.F.M., Bouwman, et al. 2001, A&A, 365, 476.Google Scholar
Shu, F.H., Adams, F.C., & Lizano, S., 1987, ARA&A, 25, 23.Google Scholar