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SpS1-Infrared spectroscopy of post-AGB objects

Published online by Cambridge University Press:  21 October 2010

Kenneth H. Hinkle ,
Sean D. Brittain  and
Richard R. Joyce
Kenneth H. Hinkle
Affiliation:
National Optical Astronomy Observatory, Tucson, AZ, USA(Operated by the Association of University for Research in Astronomy, Inc., under cooperative agreement with the National Science Foundation) email: hinkle@noao.edu, joyce@noao.edu
Sean D. Brittain
Affiliation:
Clemson University, Clemson, SC, USA email: sbritt@clemson.edu
Richard R. Joyce
Affiliation:
National Optical Astronomy Observatory, Tucson, AZ, USA(Operated by the Association of University for Research in Astronomy, Inc., under cooperative agreement with the National Science Foundation) email: hinkle@noao.edu, joyce@noao.edu
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Post-AGB (pAGB) objects are low to intermediate initial mass (≤8 M⊙) objects that have terminated normal nuclear burning and as a result are undergoing rapid evolution toward the white dwarf sequence. In classical pAGB objects evolution is to hotter effective temperatures at roughly constant luminosity. However, there are also several classes of pAGB objects that have revived nuclear burning after approaching or being on the white dwarf sequence. These include objects with delayed final helium shell flashes (e.g. Sakurai's star) and white dwarf mergers (e.g. R CrB stars). Binary evolution plays a critical role in many of these systems. A group of pAGB supergiants with large infrared excesses are suspected to be binaries that have undergone common envelope evolution. Further details on many of these objects can be found in reviews, see for instance Van Winckel (2003) and Herwig (2005).

Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 5 , Highlights H15: Highlights of Astronomy , November 2009 , pp. 548 - 549
Copyright
Copyright © International Astronomical Union 2010

References

Clayton, G. C., Geballe, T. R., Herwig, F., Fryer, C., & Asplund, M. 2007, ApJ, 662, 1220CrossRefGoogle Scholar
Clayton, G. C., Herwig, F., Geballe, T. R., Asplund, M., Tenenbaum, E. D., Engelbracht, C. W., & Gordon, K. D. 2005, ApJ, 623, L141CrossRefGoogle Scholar
De Ruyter, S., Van Winckel, H., Maas, T., Lloyd Evans, T., Waters, L. B. F. M., & Dejonghe, H. 2006, AA, 448, 641CrossRefGoogle Scholar
García-Hernández, D.A., Hinkle, K. H., Lambert, D.L., & Eriksson, K. 2009, ApJ, 696, 1733CrossRefGoogle Scholar
Herwig, F. 2005, ARA&A 43, 435Google Scholar
Hinkle, K. H., Brittain, S. D., and Lambert, D. L. 2007, ApJ, 664, 501CrossRefGoogle Scholar
Hinkle, K. H. et al. 2008, AA, 479, 817CrossRefGoogle Scholar
van Winckel, H., Waelkens, C., & Waters, L. B. F. M. 1995, AA, 293, L25Google Scholar
van Winckel, H. 2003, ARA&A 41, 391Google Scholar