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Evolution and asteroseismology of ultra-massive DA white dwarfs

Published online by Cambridge University Press:  09 October 2020

F. C. De Gerónimo
Affiliation:
Facultad de Ciencias Astronómicas y Geofísicas, Universidad Nacional de La Plata, Paseo del Bosque s/n, (1900) La Plata, Argentina email: fdegeronimo@fcaglp.unlp.edu.ar Instituto de Astrofísica La Plata, CONICET-UNLP
A. H. Córsico
Affiliation:
Facultad de Ciencias Astronómicas y Geofísicas, Universidad Nacional de La Plata, Paseo del Bosque s/n, (1900) La Plata, Argentina email: fdegeronimo@fcaglp.unlp.edu.ar Instituto de Astrofísica La Plata, CONICET-UNLP
M. E. Camisassa
Affiliation:
Facultad de Ciencias Astronómicas y Geofísicas, Universidad Nacional de La Plata, Paseo del Bosque s/n, (1900) La Plata, Argentina email: fdegeronimo@fcaglp.unlp.edu.ar Instituto de Astrofísica La Plata, CONICET-UNLP
L. G. Althaus
Affiliation:
Facultad de Ciencias Astronómicas y Geofísicas, Universidad Nacional de La Plata, Paseo del Bosque s/n, (1900) La Plata, Argentina email: fdegeronimo@fcaglp.unlp.edu.ar Instituto de Astrofísica La Plata, CONICET-UNLP

Abstract

Ultra-massive (⩾M) oxygen/neon (ONe) core white dwarfs (WDs) are the result of the evolution of isolated progenitor stars with masses above 6−M. It is expected that hydrogen-rich (DA) ultra-massive WDs harbor crystallized cores at the typical temperatures of the ZZ Ceti instability strip. These stars offer a unique opportunity to study the processes of crystallization and to infer their core chemical composition. We present a study of the evolution and asteroseismology of ultra-massive DA WDs. We found that all pulsating WDs known to date with M⩾1.1M should have more than 80% of their mass crystallized, if a ONe-core is assumed. Finally, we present a complete asteroseismological analysis to the well known ZZ Ceti BPM 37093 and a preliminary analysis to GD 518 and SDSS J0840+5222.

Type
Contributed Papers
Copyright
© International Astronomical Union 2020

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References

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