Hostname: page-component-78c5997874-g7gxr Total loading time: 0 Render date: 2024-11-19T09:19:35.915Z Has data issue: false hasContentIssue false
  • English
  • Français

Dust formation of Be stars with large infrared excess

Published online by Cambridge University Press:  12 July 2011

Chien-De Lee  and
Wen-Ping Chen
Chien-De Lee
Affiliation:
Graduate Institute of Astronomy, National Central University, Jhongli 32001, Taiwan email: [email protected]
Wen-Ping Chen
Affiliation:
Graduate Institute of Astronomy, National Central University, Jhongli 32001, Taiwan email: [email protected] Department of Physics, National Central University, Jhongli 32001, Taiwan email: [email protected]
Rights & Permissions [Opens in a new window]

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.

Classical Be stars, in addition to their emission-line spectra, are associated with infrared excess which is attributable to free-free emission from ionized gas. However, a few with exceptionally large near-infrared excess, namely with J–H, and H–Ks both greater than 0.6 mag—and excess emission extending to mid- and far-infrared wavelengths—must be accounted for by thermal emission from circumstellar dust. Evolved Be stars on the verge of turning off the main sequence may condense dust in their expanding cooling envelopes. The dust particles should be very small in size, hence reprocess starlight efficiently. This is in contrast to Herbig Ae/Be stars for which the copious infrared excess arises from relatively large grains as part of the surplus star-forming materials.

Keywords

stars: early-typestars: evolutionstars: emission-lineBestars: pre–main-sequenceinfrared: stars
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 6 , Symposium S272: Active OB stars: structure, evolution, mass loss, and critical limits , July 2010 , pp. 366 - 371
Copyright
Copyright © International Astronomical Union 2011

References

Currie, T., Hernandez, J., Irwin, J., Kenyon, S. J. et al. 2010, ApJS, 186, 191CrossRefGoogle Scholar
Currie, T., Kenyon, S. J., Balog, Z., Rieke, G. et al. 2008, ApJ, 672, 558CrossRefGoogle Scholar
Dudley, R. E. & Jeffery, C. S. 1990, MNRAS, 247, 400Google Scholar
Fabregat, J. & Torrejón, J. M. 2000, A&A, 357, 451Google Scholar
Gehrz, R. D., Hackwell, J. A. & Jones, T. W. 1974, ApJ, 191, 675CrossRefGoogle Scholar
Herbig, G. H. 1960, ApJS, 4, 337CrossRefGoogle Scholar
Mathew, B., Subramaniam, A. & Bhatt, B. C. 2008, MNRAS, 388, 1879CrossRefGoogle Scholar
Porter, J. M. & Rivinius, T. 2003, PASP, 115, 1153CrossRefGoogle Scholar
Samus, N. N, Durlevich, O. V. et al. 2004, Combined General Catalogue of Variable Stars, VizieR On-line Data Catalog: II/250Google Scholar
Schild, R. & Romanishin, W. 1976, ApJ, 204, 493CrossRefGoogle Scholar
Singh, M. & Chaubey, U. S. 1987, Ap&SS, 129, 251Google Scholar
Slettebak, A. 1985, ApJS, 59, 769CrossRefGoogle Scholar
de Winter, D., van den Ancker, M. E., Maira, A., Thé, P. S. et al. 2001, A&A, 380, 609Google Scholar
Zhang, P., Chen, P. S. & Yang, H. T. 2005, New Astron., 10, 325CrossRefGoogle Scholar