The Instability Strip for Pre--Main-Sequence Stars

Details The Instability Strip for Pre--Main-Sequence Stars The Instability Strip for Pre--Main-Sequence Stars

1998-09-21

arxiv.org/abs/astro-ph/9809254v1

Astronomy and Astrophysics

Astrophysics

14 pages, three postscript figures, accepted for publication on the Astrophysical Journal Letters

Scientific paper

10.1086/311704

We investigate the pulsational properties of Pre--Main-Sequence (PMS) stars by means of linear and nonlinear calculations. The equilibrium models were taken from models evolved from the protostellar birthline to the ZAMS for masses in the range 1 to 4 solar masses. The nonlinear analysis allows us to define the instability strip of PMS stars in the HR diagram. These models are used to constrain the internal structure of young stars and to test evolutionary models. We compare our results with observations of the best case of a pulsating young star, HR~5999, and we also identify possible candidates for pulsational variability among known Herbig Ae/Be stars which are located within or close to the instability strip boundaries.

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