Seismic evolution of low/intermediate mass PMS stars
Centro de Astrofísica da Universidade do Porto, Rua da Estrelas, 4150-762 Porto, Portugal e-mail: email@example.com
Accepted: 31 October 2007
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 4.4 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 ( ), diagrams comparing the effective temperature against the small separation can provide an alternative to Christensen-Dalsgaard (C-D) diagrams. The impact of the metal abundance of intermediate mass stars (2.5–4.4 ) has over their seismic properties is also evaluated.
Key words: stars: evolution / stars: interiors / stars: oscillations / stars: pre-main sequence
© ESO, 2008