Hostname: page-component-78c5997874-fbnjt Total loading time: 0 Render date: 2024-11-13T10:30:03.250Z Has data issue: false hasContentIssue false
  • English
  • Français

A New, Efficient Stellar Evolution Code for Calculating Complete Evolutionary Tracks

Published online by Cambridge University Press:  01 April 2008

A. Kovetz ,
O. Yaron  and
D. Prialnik
A. Kovetz
Affiliation:
Department of Geophysics and Planetary Sciences, Sackler Faculty of Exact Sciences School of Physics & Astronomy, Sackler Faculty of Exact Sciences, Tel Aviv University, Israel
O. Yaron
Affiliation:
Department of Geophysics and Planetary Sciences, Sackler Faculty of Exact Sciences
D. Prialnik
Affiliation:
Department of Geophysics and Planetary Sciences, Sackler Faculty of Exact Sciences
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.

We report on the development of a new stellar evolution code, and provide a taste of results, showing its capability to calculate full evolutionary tracks for a wide range of masses and metalicities. The code is fast and efficient, and is capable of following through all evolutionary phases, including core/shell flashes and thermal pulses, without any interruption or intervention. It is meant to be used also in the context of modeling the evolution of dense stellar systems, for performing live calculations for both ‘normal’ ZAMS/PRE-MS models, but mainly for ‘non-canonical’ stellar configurations (i.e. merger-products). We show a few examples of evolutionary calculations for stellar populations I and II, and for masses in the range 0.25–64 M⊙.

Keywords

stars: evolution(stars:) Hertzsprung-Russell diagram
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. 249 - 250
Copyright
Copyright © International Astronomical Union 2008

References

Cassisi, S., Potekhin, A. Y., Pietrinferni, A., Catelan, M., & Salaris, M. 2007 ApJ 661, 1094CrossRefGoogle Scholar
Caughlan, G. R. & Fowler, W. A. 1988, Atomic Data and Nuclear Data Tables 40, 283CrossRefGoogle Scholar
Eggleton, P. P. 1971, MNRAS 151, 351CrossRefGoogle Scholar
Ferguson, J. W., Alexander, D. R., et al. 2005 ApJ 623, 585CrossRefGoogle Scholar
Iglesias, C. A. & Rogers, F. J. 1996, ApJ 464, 943CrossRefGoogle Scholar
Itoh, N., Hayashi, H., Nishikawa, A., & Kohyama, Y. 1996 ApJS 102, 411CrossRefGoogle Scholar
Pols, O. R., Tout, C. A., Eggleton, P. P., & Han, Z. 1995, MNRAS 274, 964CrossRefGoogle Scholar
Reimers, D. 1975, MSRSL 8, 369Google Scholar