Seismic evolution of low/intermediate mass PMS stars
Centro de Astrofísica da Universidade do Porto, Rua da Estrelas, 4150-762 Porto, Portugal e-mail: fjgp@astro.up.pt
Received:
19
January
2007
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