Structure coefficients for different initial metallicities for use in stellar analysis

Structure coefficients for different initial metallicities for use in stellar analysis Internal structure coefficients for zero age Main Sequence (ZAMS) model stars with different initial metallicities are presented. A series of (Eggleton) stellar models with masses between 1 – 40 M ⊙ $1\mbox{--}40\,M_{\odot}$ and metallicities Z = 0.0001 $Z=0.0001$ , Z = 0.001 $Z=0.001$ , Z = 0.004 $Z=0.004$ , Z = 0.01 $Z=0.01$ , Z = 0.02 $Z=0.02$ , and Z = 0.03 $Z=0.03$ were used. We have also calculated the same coefficients for a recommended solar metallicity value Z = 0.0134 $Z=0.0134$ (Asplund et al. in Annu. Rev. Astron. Astrophys. 47:481, 2009). For each model, values of the internal structure constants k 2 $k_{2}$ , k 3 $k_{3}$ , k 4 $k_{4}$ and related coefficients have been derived by numerically integrating Radau’s equation with the (FORTRAN) program RADAU. The (Eggleton) stellar models used come from the ‘EZ-Web’ compilation of the Dept. of Astronomy, University of Wisconsin, Madison. The calculations follow the procedure given by Inlek and Budding (Astrophys. Space Sci. 342:365, 2012). These new results were compared with others in the literature. http://www.deepdyve.com/assets/images/DeepDyve-Logo-lg.png Astrophysics and Space Science Springer Journals

Structure coefficients for different initial metallicities for use in stellar analysis

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Publisher
Springer Netherlands
Copyright
Copyright © 2017 by Springer Science+Business Media B.V.
Subject
Physics; Astrophysics and Astroparticles; Astronomy, Observations and Techniques; Cosmology; Space Sciences (including Extraterrestrial Physics, Space Exploration and Astronautics) ; Astrobiology
ISSN
0004-640X
eISSN
1572-946X
D.O.I.
10.1007/s10509-017-3149-1
Publisher site
See Article on Publisher Site

Abstract

Internal structure coefficients for zero age Main Sequence (ZAMS) model stars with different initial metallicities are presented. A series of (Eggleton) stellar models with masses between 1 – 40 M ⊙ $1\mbox{--}40\,M_{\odot}$ and metallicities Z = 0.0001 $Z=0.0001$ , Z = 0.001 $Z=0.001$ , Z = 0.004 $Z=0.004$ , Z = 0.01 $Z=0.01$ , Z = 0.02 $Z=0.02$ , and Z = 0.03 $Z=0.03$ were used. We have also calculated the same coefficients for a recommended solar metallicity value Z = 0.0134 $Z=0.0134$ (Asplund et al. in Annu. Rev. Astron. Astrophys. 47:481, 2009). For each model, values of the internal structure constants k 2 $k_{2}$ , k 3 $k_{3}$ , k 4 $k_{4}$ and related coefficients have been derived by numerically integrating Radau’s equation with the (FORTRAN) program RADAU. The (Eggleton) stellar models used come from the ‘EZ-Web’ compilation of the Dept. of Astronomy, University of Wisconsin, Madison. The calculations follow the procedure given by Inlek and Budding (Astrophys. Space Sci. 342:365, 2012). These new results were compared with others in the literature.

Journal

Astrophysics and Space ScienceSpringer Journals

Published: Aug 22, 2017

References

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