Hostname: page-component-586b7cd67f-t8hqh Total loading time: 0 Render date: 2024-11-25T07:03:32.269Z Has data issue: false hasContentIssue false
  • English
  • Français

Changing Abundances, Changing Opacities

Published online by Cambridge University Press:  01 April 2008

Jason W. Ferguson  and
Aaron Dotter
Jason W. Ferguson
Affiliation:
Department of Physics, Wichita State University, Wichita, KS 67260-0032, USA email: [email protected]
Aaron Dotter
Affiliation:
Department of Physics and Astronomy, Dartmouth College, 6127 Wilder Laboratory, Hanover, NH 03755, USA 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.

With ever changing solar abundances being reported the equation of state and opacities needed for stellar evolution models also change. A discussion of those changes in mean molecular opacities will be presented with a discussion on the effect on evolution models. Aside from changing the abundances of the base mixture the enrichment changes too. Traditionally mean opacity tables are produced for oxygen-rich mixtures, however stars will often become carbon-rich. A discussion of carbon-rich opacities tables will also be presented.

Keywords

atomic processesequation of statemolecular processesstars: abundancesstars: evolution
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. 1 - 11
Copyright
Copyright © International Astronomical Union 2008

References

Alexander, D. R. & Ferguson, J. W. 1994, ApJ, 437, 879CrossRefGoogle Scholar
Asplund, M., Grevesse, N., Sauval, A. J., Allende Prieto, C., & Blomme, R. 2005, A&A, 431, 693Google Scholar
Dotter, A., Chaboyer, B., Ferguson, J. W., Lee, H.-C., Worthey, G., Jevremović, D., & Baron, E. 2007, ApJ, 666, 403CrossRefGoogle Scholar
Ferguson, J. W., Alexander, D. R., Allard, F., Barman, T., Bodnarik, J. G., Hauschildt, P. H., Heffner-Wong, A., & Tamanai, A. 2005, ApJ, 623, 585CrossRefGoogle Scholar
Ferguson, J. W., Heffner-Wong, A., Penley, J. J., Barman, T. S., & Alexander, D. R. 2007, ApJ, 666, 261CrossRefGoogle Scholar
Grevesse, N. & Noels, A. 1993, Origin and Evolution of the ElementsGoogle Scholar
Grevesse, N. & Sauval, A. J. 1998, Sp.Sci.Rev, 85, 161CrossRefGoogle Scholar
Iglesias, C. A. & Rogers, F. J. 1991, ApJ, 371, 408CrossRefGoogle Scholar
Iglesias, C. A. & Rogers, F. J. 1993, ApJ, 412, 752CrossRefGoogle Scholar
Iglesias, C. A. & Rogers, F. J. 1996, ApJ, 464, 943CrossRefGoogle Scholar
Lederer, M. T. & Aringer, B. 2008, AIPC, 1001, 11Google Scholar
Lodders, K. 2003, ApJ, 591, 1220CrossRefGoogle Scholar
Marigo, P. 2002, A&A, 387, 507Google Scholar
Seaton, M. J., Yan, Y., Mihalas, D., & Pradhan, A. K. 1994, MNRAS, 266, 805CrossRefGoogle Scholar
Tennyson, J., Harris, G. J., Barber, R. J., La Delfa, S., Voronin, B. A., Kaminsky, B. M., & Pavlenko, Ya. V. 2007, Mol. Phys., 105, 701CrossRefGoogle Scholar