Seismic evolution of low/intermediate mass PMS stars

TL;DR

This study investigates the internal structure and seismic characteristics of low/intermediate mass PMS stars using stellar models, revealing new diagnostic diagrams and effects of metallicity on seismic properties.

Contribution

It introduces alternative seismic diagnostic diagrams for intermediate-mass PMS stars and evaluates the impact of metallicity on their seismic features.

Findings

Effective temperature vs. small separation diagrams as alternatives to C-D diagrams.

Metallicity significantly influences seismic properties of intermediate-mass PMS stars.

Seismic and non-seismic properties analyzed across a range of stellar masses and evolutionary stages.

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.