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The evolution of ‘the moment of inertia’ of stars

Published online by Cambridge University Press:  01 April 2008

Y.-C. Kim  and
S. Barnes
Y.-C. Kim
Affiliation:
Astronomy Department, Yonsei University, Seoul, 120-749, Korea email: yckim@yonsei.ac.kr
S. Barnes
Affiliation:
Lowell Observatory, Flagstaff, AZ 86001, USA email: barnes@lowell.edu
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Abstract

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Observations of the rotation periods of cool open cluster stars display a distinctive dichotomy when plotted against stellar mass/color. Other measures of stellar activity are also known to be dependent on stellar mass and structure, especially the onset and characteristics of convection zones. One proposal for understanding the observed rotation period dichotomy suggested dependencies on the moment of inertia of either the whole star or that of only the outer convection zone (Barnes 2003).

The moment of inertia of stars with the mass between 0.1Msun and 3.0Msun have been calculated using a version of Yale Stellar evolution code (aka YREC). Each star has been evolved from stellar birthline to the onset of the core He burning. For easy comparison to observations, we have calculated the isochrones of these quantities as well as the convective turnover time, of interest to the activity community.

Keywords

stars: interiors stars: 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. 117 - 118
Copyright
Copyright © International Astronomical Union 2008

References

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