Seismic evolution of low/intermediate mass PMS stars

Details Seismic evolution of low/intermediate mass PMS stars Seismic evolution of low/intermediate mass PMS stars

2007-12-05

arxiv.org/abs/0712.0725v1

Astronomy and Astrophysics

Astrophysics

4 pages, 5 figures, accepted for publication on A&A

Scientific paper

10.1051/0004-6361:20077136

This article presents a study of the evolution of the internal structure and seismic properties expected for low/intermediate mass Pre-Main Sequence (PMS) stars. Seismic and non-seismic properties of PMS stars were analysed. This was done using 0.8 to 4.4M$_\odot$ stellar models at stages ranging from the end of the Hayashi track up to the Zero-Age Main-Sequence (ZAMS). This research concludes that, for intermediate-mass stars (M$>$1.3M$_\odot$), diagrams comparing the effective temperature ($T_{eff}$) against the small separation can provide an alternative to Christensen-Dalsgaard (C-D) diagrams. The impact of the metal abundance of intermediate mass stars (2.5-4.4M$_\odot$) has over their seismic properties is also evaluated.

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