Hostname: page-component-76fb5796d-r6qrq Total loading time: 0 Render date: 2024-04-26T14:53:18.968Z Has data issue: false hasContentIssue false
  • English
  • Français

Non-LTE Spectral Analysis of Extremely Hot Post-AGB Stars: Constraints for Evolutionary Theory

Published online by Cambridge University Press:  01 April 2008

Thomas Rauch ,
Klaus Werner ,
Marc Ziegler ,
Lars Koesterke  and
Jeffrey W. Kruk
Thomas Rauch
Affiliation:
Institute for Astronomy and Astrophysics, Kepler Center for Astro and Particle Physics, Eberhard Karls University, Sand 1, 72076 Tübingen, Germany e-mail: rauch@astro.uni-tuebingen.de
Klaus Werner
Affiliation:
Institute for Astronomy and Astrophysics, Kepler Center for Astro and Particle Physics, Eberhard Karls University, Sand 1, 72076 Tübingen, Germany e-mail: rauch@astro.uni-tuebingen.de
Marc Ziegler
Affiliation:
Institute for Astronomy and Astrophysics, Kepler Center for Astro and Particle Physics, Eberhard Karls University, Sand 1, 72076 Tübingen, Germany e-mail: rauch@astro.uni-tuebingen.de
Lars Koesterke
Affiliation:
Texas Advanced Computer Center, University of Texas, Austin, TX 78712, USA
Jeffrey W. Kruk
Affiliation:
Department of Physics and Astronomy, Johns Hopkins University, Baltimore, MD 21218, USA
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.

Spectral analysis by means of Non-LTE model-atmosphere techniques has arrived at a high level of sophistication: fully line-blanketed model atmospheres which consider opacities of all elements from H to Ni allow the reliable determination of photospheric parameters of hot, compact stars. Such models provide a crucial test of stellar evolutionary theory: recent abundance determinations of trace elements like, e.g., F, Ne, Mg, P, S, Ar, Fe, and Ni are suited to investigate on AGB nucleosynthesis. E.g., the strong Fe depletion found in hydrogen-deficient post-AGB stars is a clear indication of an efficient s-process on the AGB where Fe is transformed into Ni or even heavier trans iron-group elements. We present results of recent spectral analyses based on high-resolution UV observations of hot stars.

Keywords

astronomical data bases: miscellaneousatomic dataline: identificationstars: abundancesstars: AGB and post-AGBstars: atmospheresstars: early-typestars: evolution(stars:) white dwarfs
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 4 , Symposium S252: The Art of Modeling Stars in the 21st Century , April 2008 , pp. 223 - 228
Copyright
Copyright © International Astronomical Union 2008

References

Asplund, M., Grevesse, N., & Sauval, A. J. 2005, in: Cosmic Abundances Records of Stellar Evolution and Nucleosynthesis, eds. Barnes, T. G. III., & Bash, F. N., The ASP Conference Series Vol. 336 (San Francisco ASP), p. 25Google Scholar
Dreizler, S., Werner, K., & Heber, U. 1995, in: White Dwarfs, eds. Koester, D., & Werner, K., LNP, 443, 160Google Scholar
Hébrard, G., et al. 2002, ApJS, 140, 103CrossRefGoogle Scholar
Herald, J. E., Bianchi, L., & Hillier, D. J. 2005, ApJ, 627, 424CrossRefGoogle Scholar
Hubeny, I. 2003, in: Stellar Atmosphere Modeling, eds. Hubeny, I., Mihalas, D., & Werner, K., The ASP Conference Series Vol. 288 (San Francisco ASP), p. 51Google Scholar
Iben, I. Jr., & Tutukov, A. V. 1985, ApJS, 58, 661CrossRefGoogle Scholar
Iben, I. Jr., Kaler, J. B., Truran, J. W., & Renzini, A. 1983, ApJ, 264, 605CrossRefGoogle Scholar
Jahn, D., Rauch, T., Reiff, E., Werner, K., Kruk, J. W., Dreizler, S., & Herwig, F. 2007, A&A, 462, 281Google Scholar
Johnston, W. D. & Kunze, H.-J. 1969, ApJ, 157, 1469CrossRefGoogle Scholar
König, R., Kolk, K.-H., & Kunze, H.-J. 1993, Physica Scripta 48, 9CrossRefGoogle Scholar
Kramida, A. E. & Buchet-Poulizac, M.-C. 2006, Eur. Phys. J. D, 39, 173CrossRefGoogle Scholar
Lanz, T. & Hubeny, I. 2003, in: Stellar Atmosphere Modeling, eds. Hubeny, I., Mihalas, D., & Werner, K., The ASP Conference Series Vol. 288 (San FranciscoASP), p. 117Google Scholar
Lemoine, M., et al. 2002, ApJS, 140, 67CrossRefGoogle Scholar
Lugaro, M., Ugalde, C., & Karakas, A. I., et al. 2004, ApJ, 615, L934CrossRefGoogle Scholar
Miksa, S., Deetjen, J. L., Dreizler, S., Kruk, J. W., Rauch, T., & Werner, K. 2002, A&A 389, 953Google Scholar
Rauch, T. 1997, A&A, 320, 237Google Scholar
Rauch, T. 2003, A&A, 403, 709Google Scholar
Rauch, T., & Deetjen, J. L. 2003, in: Stellar Atmosphere Modeling, eds. Hubeny, I., Mihalas, D., & Werner, K., The ASP Conference Series Vol. 288 (San Francisco ASP), p. 103Google Scholar
Rauch, T., Ziegler, M., Werner, K., et al. 2007, A&A, 470, 317Google Scholar
Werner, K. 1986, A&A, 161, 177Google Scholar
Werner, K. 1989, A&A, 226, 265Google Scholar
Werner, K. & Herwig, F. 2006, PASP, 118, 183CrossRefGoogle Scholar
Werner, K., Deetjen, J. L., Dreizler, , et al. 2003, in: Stellar Atmosphere Modeling, eds. Hubeny, I., Mihalas, D., & Werner, K., The ASP Conference Series Vol. 288 (San Francisco ASP), p. 31Google Scholar
Werner, K. & Rauch, T. 1994, A&A, 284, L5Google Scholar
Werner, K., Rauch, T., Reiff, E., Kruk, J. W., & Napiwotzki, R. 2004, A&A, 427, 685Google Scholar
Werner, K., Rauch, T., & Kruk, J. W. 2005, A&A, 433, 641Google Scholar
Werner, K., Rauch, T., & Kruk, J. W. 2007a, A&A, 466, 317Google Scholar
Werner, K., Rauch, T., & Kruk, J. W. 2007b, A&A, 481, 807Google Scholar