How Massive Single Stars End Their Life

@article{Heger2003HowMS,
  title={How Massive Single Stars End Their Life},
  author={Alexander Heger and Chris L. Fryer and S. E. Woosley and Norbert Langer and Dieter H. Hartmann},
  journal={The Astrophysical Journal},
  year={2003},
  volume={591},
  pages={288-300}
}
How massive stars die—what sort of explosion and remnant each produces—depends chiefly on the masses of their helium cores and hydrogen envelopes at death. For single stars, stellar winds are the only means of mass loss, and these are a function of the metallicity of the star. We discuss how metallicity, and a simplified prescription for its effect on mass loss, affects the evolution and final fate of massive stars. We map, as a function of mass and metallicity, where black holes and neutron… Expand
The Formation and Evolution of Very Massive Stars in Dense Stellar Systems
Abstract The early evolution of dense stellar systems is governed by massive single star and binary evolution. Core collapse of dense massive star clusters can lead to the formation of very massiveExpand
Astrophysics: Different stellar demise
TLDR
Analysis of the spectrum and light curve of supernova 2007bi, a luminous event in a nearby dwarf galaxy, provides evidence of such an explosion and suggests that there are extremely massive stars in the local Universe that could provide astronomers with a close-up of the type of star that may have dominated the early Universe. Expand
The Final Stages of Massive Star Evolution and Their Supernovae
In this chapter I discuss the final stages in the evolution of massive stars – stars that are massive enough to burn nuclear fuel all the way to iron group elements in their core. The core eventuallyExpand
Asteroseismology of High-Mass Stars: New Insights of Stellar Interiors With Space Telescopes
  • D. Bowman
  • Physics
  • Frontiers in Astronomy and Space Sciences
  • 2020
Massive stars are important metal factories in the Universe. They have short and energetic lives, and many of them inevitably explode as a supernova and become a neutron star or black hole. In turn,Expand
The Impact of Interacting Binary Stars on Core-collapse Supernovae and Emission Nebulae
The evolution of binary-star systems vary from that of single stars as they can interact with their companions. This leads to mass loss, mass gain, or stellar mergers. We now know that most massiveExpand
Mass loss and fate of the most massive stars
  • J. Vink
  • Physics
  • Proceedings of the International Astronomical Union
  • 2011
Abstract The fate of massive stars up to 300M⊙ is highly uncertain. Do these objects produce pair-instability explosions, or normal Type Ic supernovae? In order to address these questions, we need toExpand
Progenitors of Core-Collapse Supernovae
Abstract Massive stars have a strong impact on their surroundings, in particular when they produce a core-collapse supernova at the end of their evolution. In these proceedings, we review the generalExpand
Mass-loss predictions for evolved very metal-poor massive stars
Context. The first couple of stellar generations may have been massive, of order 100 M� , and to have played a dominant role in galaxy formation and the chemical enrichment of the early Universe.Expand
Two White Dwarfs with Oxygen-Rich Atmospheres
TLDR
The detection of two white dwarfs with large photospheric oxygen abundances are reported, implying that they are bare oxygen-neon cores and that they may have descended from the most massive progenitors that avoid core collapse. Expand
First stars. II. Evolution with mass loss
The first stars are assumed to be predominantly massive. Although, due to the low initial abundances of heavy elements the line-driven stellar winds are supposed to be inefficient in the first stars,Expand
...
1
2
3
4
5
...

References

SHOWING 1-10 OF 77 REFERENCES
The evolution and explosion of massive stars
Like all true stars, massive stars are gravitationally confined thermonuclear reactors whose composition evolves as energy is lost to radiation and neutrinos. Unlike lower-mass stars (M≲8M⊙),Expand
Evolution and explosion of very massive primordial stars
While the modern stellar IMF shows a rapid decline with increasing mass, theoretical investigations suggest that very massive stars (>100 solar masses) may have been abundant in the early universe.Expand
Pair-Instability Supernovae, Gravity Waves, and Gamma-Ray Transients
Growing evidence suggests that the first generation of stars may have been quite massive (~100-300 M☉). If they retain their high mass until death, such stars will, after about 3 Myr, makeExpand
First Stars, Very Massive Black Holes, and Metals
Recent studies suggest that the initial mass function (IMF) of the first stars (Population III) is likely to have been extremely top-heavy, unlike what is observed at present. We propose a scenarioExpand
On the Stability of Very Massive Primordial Stars
The stability of metal-free very massive stars (Z \ 0; M \ 120¨500 is analyzed and compared M _ ) with metal-enriched stars. Such zero-metallicity stars are unstable to nuclear-powered radialExpand
The pre-supernova evolution of rotating massive stars
Massive stars are born rotating rigidly with a significant fraction of critical rotation at the surface. Consequently, rotationally-induced circulation and instabilities lead to chemical mixing inExpand
Mass Limits For Black Hole Formation
We present a series of two-dimensional core-collapse supernova simulations for a range of progenitor masses and different input physics. These models predict a range of supernova energies and compactExpand
Formation Rates of Black Hole Accretion Disk Gamma-Ray Bursts
The cosmological origin of at least an appreciable fraction of classical gamma-ray bursts (GRBs) is now supported by redshift measurements for a half-dozen faint host galaxies. Still, the nature ofExpand
The Nucleosynthetic Signature of Population III
Growing evidence suggests that the first generation of stars may have been quite massive (~100-300 M?). Could these stars have left a distinct nucleosynthetic signature? We explore theExpand
Forming the First Stars in the Universe: The Fragmentation of Primordial Gas.
TLDR
This work investigates the fragmentation properties of metal-free gas in the context of a hierarchical model of structure formation and finds that the gas dissipatively settles into a rotationally supported disk that has a very filamentary morphology. Expand
...
1
2
3
4
5
...