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EC14026 Stars: Theoretical Considerations

Published online by Cambridge University Press:  08 February 2017

G. Fontaine ,
S. Charpinet ,
P. Brassard ,
P. Chayer ,
F.J. Rogers ,
C.A. Iglesias  and
B. Dorman
G. Fontaine
Affiliation:
Département de Physique, Université de Montréal, Montréal, Qu ébec, Canada E3C 3J7
S. Charpinet
Affiliation:
Département de Physique, Université de Montréal, Montréal, Qu ébec, Canada E3C 3J7
P. Brassard
Affiliation:
Département de Physique, Université de Montréal, Montréal, Qu ébec, Canada E3C 3J7
P. Chayer
Affiliation:
Center for EUV Astrophysics, University of California, Berkeley, California 94720, U.S.A.
F.J. Rogers
Affiliation:
Lawrence Livermore National Laboratory, Livermore, California 94550, U.S.A.
C.A. Iglesias
Affiliation:
Lawrence Livermore National Laboratory, Livermore, California 94550, U.S.A.
B. Dorman
Affiliation:
Laboratory for Astronomy and Solar Physics, NASA/GSFC, Greenbelt, Maryland 20771, U.S.A.

Extract

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The recent discovery of pulsating subdwarf B (sdB) stars at the South African Astronomical Observatory (Kilkenny et al. 1997; Koen et al. 1997; Stobie et al. 1997; O'Donoghue et al. 1997) has opened a brand new avenue in the field of asteroseismology. The study of these pulsators (dubbed EC14026 stars, after the prototype) offers the exciting possibility of exploiting the full power of asteroseismology to investigate the sdB phase of stellar evolution, one of the last frontiers in our general understanding of the history of stars.

Type
VI. Asteroseismology II
Information
Symposium - International Astronomical Union , Volume 185: New Eyes to See Inside the Sun and Stars , 1998 , pp. 367 - 374
Copyright
Copyright © Kluwer 1998 

References

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