Spectroscopic monitoring of the luminous blue variable Westerlund1-243 from 2002 to 2009

TL;DR

This study presents a detailed spectroscopic monitoring of the luminous blue variable W243 over several years, revealing its spectral evolution, surface composition, and mass-loss behavior, contributing to understanding LBV variability and evolution.

Contribution

It provides the first long-term high-resolution spectroscopic dataset of W243, showing its spectral transformation and surface chemical enrichment, highlighting LBV variability and mass-loss processes.

Findings

W243 evolved from a B2Ia to an A3Ia+ spectral type.

Surface shows nitrogen enrichment and carbon/oxygen depletion.

Star exhibits photospheric pulsations and episodic mass loss.

Abstract

The massive post-Main Sequence star W243 in the galactic starburst cluster Westerlund 1 has undergone a spectral transformation from a B2Ia supergiant devoid of emission features in 1981 to an A-type supergiant with a rich emission-line spectrum by 2002/03. We used VLT/UVES and VLT/FLAMES to obtain high-resolution spectra on six epochs in 2003/04 (UVES) and ten epochs in 2008/09 (FLAMES). These spectra are used alongside other VLT/FLAMES and NTT/EMMI spectra to follow the evolution of W243 from 2002 to 2009. W243 displays a complex, time-varying spectrum with emission lines of Hydrogen, Helium and Lyman-pumped metals, forbidden lines of Nitrogen and Iron, and a large number of absorption lines from neutral and singly-ionized metals. Many lines are complex emission/absorption blends. The LBV has a current temperature of ~8500K (spectral type A3Ia+), and displays signs of photospheric pulsations and weak episodic mass loss. Nitrogen is highly overabundant, with Carbon and Oxygen depleted, indicative of surface CNO-processed material and considerable previous mass-loss, although current time-averaged mass-loss rates are low. The emission-line spectrum forms at large radii, when material lost by the LBV in a previous mass-loss event is ionized by an unseen hot companion. Monitoring of the near-infrared spectrum suggests that the star has not changed significantly since it finished evolving to the cool state, close to the Humphreys-Davidson limit, in early 2003. [ABRIDGED]