Seismic evolution of low/intermediate mass PMS stars

Abstract

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.

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

References in corpus (1)

• Discovery of $\delta$ Scuti pulsation in the Herbig Ae star VV Ser