Mass loss and stellar superwinds

Abstract

Mass loss bridges the gap between massive stars and supernovae (SNe) in two major ways: (i) theoretically it is the amount of mass lost that determines the mass of the star prior to explosion, and (ii) observations of the circumstellar material around SNe may teach us the type of progenitor that made the SN. Here, I present the latest models and observations of mass loss from massive stars, both for canonical massive O stars, as well as very massive stars (VMS) that show Wolf-Rayet type features.

12 pages, 9 figures. Invited Review in: Bridging the gap: from massive stars to supernovae (Royal Society Meeting)

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Cited by in corpus (12)

• Very massive stars, pair-instability supernovae and intermediate-mass black holes with the SEVN code
• Merging black hole binaries: the effects of progenitor's metallicity, mass-loss rate and Eddington factor
• Cygnus X-1 contains a 21-solar mass black hole -- implications for massive star winds
• Merging black holes in young star clusters
• Rates of Compact Object Coalescences
• The cosmic merger rate of stellar black hole binaries from the Illustris simulation
• Host galaxies of merging compact objects: mass, star formation rate, metallicity and colours
• MOCCA-SURVEY database I. Accreting white dwarf binary systems in globular clusters -- IV. cataclysmic variables -- properties of bright and faint populations
• The star clusters that make black hole binaries across cosmic time
• Evolution of massive stellar triples and implications for compact object binary formation
• Centrifugally Driven Mass Loss and Outbursts of Massive Stars
• Bridging the Gap: From Massive Stars to Supernovae