2008年2月13日 · We show that the masses of WNH stars are systematically higher than H-poor WR stars (both WN and WC), with little overlap, while H mass fractions of luminous WNH stars …

2017年9月18日 · The luminous blue variable (LBV) phase of evolution, punctuated by eruptive mass loss, is thought to be important in the mass-loss evolution of massive stars [1,2]. …

Wolf–Rayet stars, often abbreviated as WR stars, are a rare heterogeneous set of stars with unusual spectra showing prominent broad emission lines of ionised helium and highly ionised …

We propose the new designation ‘‘WNH’’ for luminous Wolf-Rayet (WR) stars of the nitrogen sequence with hydrogen in their spectra. These have been commonly referred to as WNL …

We propose the new designation "WNH" for luminous Wolf-Rayet (WR) stars of the nitrogen sequence with hydrogen in their spectra. These have been commonly referred to as WNL …

We propose the new designation "WNH" for luminous Wolf-Rayet (WR) stars of the nitrogen sequence with hydrogen in their spectra. These have been commonly referred to as WNL …

Massive stars play a major role in the evolution of their host galaxies, and serve as important probes of the distant Universe. It has been established that the majority of massive stars …

2008年2月12日 · We show that the masses of WNH stars are systematically higher than H-poor WR stars (both WN and WC), with little overlap, while H mass fractions of luminous WNH stars …

2018年2月5日 · Proximity to the Eddington limit may also lead to eruptive mass loss in luminous blue variable (LBV) Eta Car type giant eruptions (e.g. Shaviv 2000; Smith & Owocki 2006; …

scientific article published in the Astrophysical Journal. On the Role of the WNH Phase in the Evolution of Very Massive Stars: Enabling the LBV Instability with Feedback (Q55879136)