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Pulsation of PMS 1.8 M⊙ Stars: A Theoretical Investigation

Published online by Cambridge University Press:  08 February 2017

Doru Marian Suran
Doru Marian Suran*
Affiliation:
ASTRONOMICAL INSTITUTE OF ROMANIAN ACADEMY, Str. Cutitul de Argint, No.5, 75212 Bucharest 28, ROMANIA, e-mail: suran@roastro.astro.ro

Extract

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Herbig Ae stars are pre-main sequence of masses ~2M⊙. As they trace their course toward the ZAMS, they cross the classical instability strip. At this stage, their evolution has considerably slowed down. Their structure differs from that of stars evolving after the ZAMS (δ Scuti stars) in the very deep layers where nuclear burning has only recently started. But the outer layers for stars before and after the ZAMS are expected to be similar. As these layers drive the pulsation of δ Scuti stars, it is reasonable to expect that PMS stars in the instability strip also are destabilized by the κ mechanism with a similar range of unstable modes. Indeed, recently a Herbig Ae star has been reported as a variable (Kurtz and Marang 1995).

Type
VI. Asteroseismology II
Information
Symposium - International Astronomical Union , Volume 185: New Eyes to See Inside the Sun and Stars , 1998 , pp. 397 - 398
Copyright
Copyright © Kluwer 1998 

References

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