EDP Sciences
Free access
Volume 478, Number 1, January IV 2008
Page(s) 193 - 196
Section Stellar structure and evolution
DOI http://dx.doi.org/10.1051/0004-6361:20077136

A&A 478, 193-196 (2008)
DOI: 10.1051/0004-6361:20077136

Seismic evolution of low/intermediate mass PMS stars

F. J. G. Pinheiro

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 $M_\odot$ 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 > 1.3 $M_\odot$), diagrams comparing the effective temperature $(T_{\rm eff})$ against the small separation can provide an alternative to Christensen-Dalsgaard (C-D) diagrams. The impact of the metal abundance of intermediate mass stars (2.5-4.4 $M_\odot$) has over their seismic properties is also evaluated.

Key words: stars: evolution -- stars: interiors -- stars: oscillations -- stars: pre-main sequence

© ESO 2008