Hostname: page-component-848d4c4894-r5zm4 Total loading time: 0 Render date: 2024-06-22T10:36:30.907Z Has data issue: false hasContentIssue false
  • English
  • Français

Extended Dust Shells around Carbon Stars in the Infrared and in Optical Light

Published online by Cambridge University Press:  25 May 2016

Hideyuki Izumiura ,
L.B.F.M. Waters ,
T. De Jong ,
C. Loup  and
O. Hashimoto
Hideyuki Izumiura
Affiliation:
Okayama Astrophysical Observatory, NAOJ, Kamogata, Asakuchi, Okayama 719-0232, Japan
L.B.F.M. Waters
Affiliation:
Astronomical Institute “Anton Pannekoek”, University of Amsterdam, NL-1098 SJ Amsterdam, The Netherlands
T. De Jong
Affiliation:
Astronomical Institute “Anton Pannekoek”, University of Amsterdam, NL-1098 SJ Amsterdam, The Netherlands
C. Loup
Affiliation:
Institut d'Astrophysique de Paris, CNRS, 75014 Paris, France
O. Hashimoto
Affiliation:
Gunma Astronomical Observatory, 1-18-7 Ohotomo, Maebashi, Gunma 371, Japan

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 investigate the structure of extended dust shells around optical carbon stars in the far-infrared and in optical light. In the optical we have discovered that R Scl and U Ant are associated with circularly extended emission, the radii of which are about 20″ and 58″, respectively. The emission is probably scattered light of the central star by dust grains in their circumstellar shells. In the far-infrared we have discovered a double shell structure surrounding U Ant in high resolution IRAS images, which is direct evidence of a periodic change of mass-loss on a time-scale of the order of 104 years in the AGB evolution. Relating the two shells to two consecutive thermal pulses allows for a self-consistent determination of the interpulse period, core-mass, luminosity, and distance. Direct mapping of Y CVn at 90 and 160 μm with ISOPHOT on board ISO has revealed a very extended detached dust shell around this star. The mass-loss rate is found to have decreased drastically by two orders of magnitude 1.4×104 years ago, which should be an important clue to the understanding of J-type stars.

Type
Session IX — Circumstellar Emission and Environment
Information
Symposium - International Astronomical Union , Volume 177: The Carbon Star Phenomenon , 2000 , pp. 425 - 432
Copyright
Copyright © Kluwer 2000 

References

Bontekoe, Tj. R., Koper, E. & Kester, D. J. M. 1994, A&Ap, 284, 1037 Google Scholar
Gilman, R. C. 1972, ApJ, 178, 423 Google Scholar
Goldreich, P. & Scoville, N. 1976, ApJ, 205, 144 Google Scholar
Huggins, P. J., Olofsson, H. & Johansson, L. E. B. 1988, ApJ, 332, 1009 CrossRefGoogle Scholar
Iben, I. Jr. & Renzini, A. 1983, Ann. Rev. Astron. Astrophys., 21, 271 Google Scholar
Izumiura, H., Hashimoto, O., Kawara, K., Yamamura, I. & Waters, L. B. F. M. 1996, A&Ap, 315, L221 Google Scholar
Izumiura, H., Kester, D. J. M., de Jong, T., Loup, C., Waters, L. B. F. M. & Bontekoe, Tj.R. 1995, Ap&;SS, 224, 495 Google Scholar
Izumiura, H., Waters, L. B. F. M., de Jong, T., Loup, C., Bontekoe, Tj. R. & Kester, D. J. M. 1997, A&Ap, 323, 449 Google Scholar
Kwan, J. & Hill, F. 1977, ApJ, 215, 781 Google Scholar
Lemke, D., Klaas, U., Abolins, J., et al. 1996, A&Ap, 315, L64 Google Scholar
Olofsson, H., Bergman, P., Eriksson, K. & Gustafsson, B. 1996, A&Ap, 311, 587 Google Scholar
Paczyński, B. 1975, ApJ, 202, 558 CrossRefGoogle Scholar
Sopka, R. J., Hildebrand, R., Jaffe, D. T., Gatley, I., Roellig, T., Werner, M., Jura, M. & Zuckerman, B. 1985, ApJ, 294, 242 CrossRefGoogle Scholar