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Pulsating white dwarfs and convection

Published online by Cambridge University Press:  09 October 2020

J. L. Provencal Open the ORCID record for J. L. Provencal [Opens in a new window] ,
M. H. Montgomery Open the ORCID record for M. H. Montgomery [Opens in a new window] ,
H. L. Shipman  and
The WET Team
J. L. Provencal
Affiliation:
University of Delaware, Dept. of Physics and Astronomy, Newark, DE19716 email: jlp@udel.edu
M. H. Montgomery
Affiliation:
Dept. of Astronomy & University of Texas, Austin, TX email: mikemon@astro.as.utexas.edu
H. L. Shipman
Affiliation:
University of Delaware, Dept. of Physics and Astronomy, Newark, DE19716 email: jlp@udel.edu
The WET Team
Affiliation:
See www.physics.udel.edu/darc for a list of WET collaborators
Rights & Permissions [Opens in a new window]

Abstract

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Convection is a highly turbulent, three dimensional process that is traditionally treated using a simple, local, time independent description. Convection is one of the largest sources of theoretical uncertainty in stellar modeling. We outline recent progress in studies using pulsating white dwarfs to constrain convection and calibrate mixing length theory.

Keywords

convectionwhite dwarfsoscillations
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 15 , Symposium S357: White Dwarfs as Probes of Fundamental Physics: Tracers of Planetary, Stellar and Galactic Evolution , October 2019 , pp. 127 - 130
Copyright
© International Astronomical Union 2020

References

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