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What asteroseismology can teach us about low-mass core helium burning models

Published online by Cambridge University Press:  18 February 2014

Thomas N. Constantino ,
Simon W. Campbell  and
John C. Lattanzio
Thomas N. Constantino
Affiliation:
Monash Centre for Astrophysics, School of Mathematical Sciencies Monash University, Victoria 3800, Australia email: thomas.constantino@monash.edu
Simon W. Campbell
Affiliation:
Monash Centre for Astrophysics, School of Mathematical Sciencies Monash University, Victoria 3800, Australia email: thomas.constantino@monash.edu
John C. Lattanzio
Affiliation:
Monash Centre for Astrophysics, School of Mathematical Sciencies Monash University, Victoria 3800, Australia email: thomas.constantino@monash.edu
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Abstract

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Standard models of low-mass core helium burning stars typically give an asymptotic l=1 g-mode period spacing well below that inferred from observed mixed modes. We find that most physical uncertainties, such as mixing beyond the fully convective core, are not significant enough to be responsible for such a discrepancy. The solution to the problem may lie in a deviation of structure away from its canonical form, such as a more massive H-exhausted core, which we briefly explore here.

Keywords

stars: horizontal-branchstars: interiorsstars: late-typestars: oscillations
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 9 , Symposium S301: Precision Asteroseismology , August 2013 , pp. 399 - 400
Copyright
Copyright © International Astronomical Union 2014 

References

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