On the evolutionary status of Be stars. I. Field Be stars near the Sun

TL;DR

This study investigates the evolutionary status of field Be stars near the Sun by analyzing a sample of 97 stars, accounting for rotation effects, and determining their ages and masses using models for rotating stars.

Contribution

It introduces a method combining spectrophotometry and rotating stellar models to estimate ages and masses of Be stars, revealing a mass-dependent distribution of their evolutionary stages.

Findings

Be stars are spread across the entire main sequence phase.

Massive Be stars show the phenomenon at earlier evolutionary stages.

Higher mass-loss rates and angular momentum transport influence Be star evolution.

Abstract

A sample of 97 galactic field Be stars were studied by taking into account the effects induced by the fast rotation on their fundamental parameters. All program stars were observed in the BCD spectrophotometric system in order to minimize the perturbations produced by the circumstellar environment on the spectral photospheric signatures. This is one of the first attempts at determining stellar masses and ages by simultaneously using model atmospheres and evolutionary tracks, both calculated for rotating objects. The stellar ages ($\tau$) normalized to the respective inferred time that each rotating star can spend in the main sequence phase ($\tau\_{\rm MS}$) reveal a mass-dependent trend. This trend shows that: a) there are Be stars spread over the whole interval $0 \la \tau/\tau\_{\rm MS} \la 1$ of the main sequence evolutionary phase; b) the distribution of points in the ($\tau/\tau\_{\rm MS},M/M\_{\odot}$) diagram indicates that in massive stars ($M \ga 12M\_{\odot}$) the Be phenomenon is present at smaller $\tau/\tau\_{\rm MS}$ age ratios than for less massive stars ($M \la 12M\_{\odot}$). This distribution can be due to: $i$) higher mass-loss rates in massive objets, which can act to reduce the surface fast rotation; $ii$) circulation time scales to transport angular momentum from the core to the surface, which are longer the lower the stellar mass.