Presupernova Evolution of Rotating Massive Stars. I. Numerical Method and Evolution of the Internal Stellar Structure

@article{Heger2000PresupernovaEO,
  title={Presupernova Evolution of Rotating Massive Stars. I. Numerical Method and Evolution of the Internal Stellar Structure},
  author={Alexander Heger and Norbert Langer and S. E. Woosley Ucsc and Mpa and Universitaet Potsdam},
  journal={The Astrophysical Journal},
  year={2000},
  volume={528},
  pages={368-396}
}
The evolution of rotating stars with zero-age main-sequence (ZAMS) masses in the range 8-25 M☉ is followed through all stages of stable evolution. The initial angular momentum is chosen such that the star's equatorial rotational velocity on the ZAMS ranges from zero to ~ 70% of breakup. The stars rotate rigidly on the ZAMS as a consequence of angular momentum redistribution during the pre-main-sequence evolution. Redistribution of angular momentum and chemical species are then followed as a… Expand
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References

SHOWING 1-10 OF 67 REFERENCES
Evolution of rotating stars. II. Calculations with time-dependent redistribution of angular momentum for 7 and 10 M/sub sun/ stars
Calculations have been performed for the evolution of rotating stars with realistic, time-dependent redistribution of angular momentum and chemical composition due to gas-dynamical instabilities.Expand
The evolution of rotating stars. I - Method and exploratory calculations for a 7-solar-mass star
A method is developed which allows us to study the evolution of rotating stars well beyond the main-sequence stage. We consider four different cases of redistribution of angular momentum in anExpand
Evolutionary sequences of stellar models of intermediate and high mass including convective core overshooting
Stellar evolution with parameterized overshooting from the convective core has been studied for the stellar mass range M/M(solar) = 3-30 and for the initial chemical composition range Xe =Expand
Internal rotation of the Sun
The low surface rotation rate of the Sun and other main-sequence stars is believed to be the result of angular momentum loss due to a stellar wind1. This loss also leads to a differential rotation,Expand
Gravitational waves from hot young rapidly rotating neutron stars
Gravitational radiation drives an instability in the r-modes of young rapidly rotating neutron stars. This instability is expected to carry away most of the angular momentum of the star byExpand
Presupernova evolution of massive stars.
Population I stars of 15 M/sub sun/ and 25 M/sub sun/ have been evolved from the zero-age main sequence through iron core collapse utilizing a numerical model that incorporates both implicitExpand
Birth kicks as the origin of pulsar rotation
Radio pulsars are thought to born with spin periods of 0.02–0.5 s and space velocities of 100–1,000 km s−1, and they are inferred to have initial dipole magnetic fields of 1011–1013 G (refs 1–5). TheExpand
Inhibition of Wind Compressed Disk Formation by Nonradial Line-Forces
We investigate the effects of nonradial line forces on the formation of a wind-compressed disk (WCD) around a rapidly rotating B star. Such nonradial forces can arise both from asymmetries in theExpand
Evolutionary models of the rotating sun
This paper reviews current work on the evolution of a differentially rotating solar model. Although we discuss global features of the evolution with rotation in general terms, the specific modelsExpand
Collapsars: Gamma-ray bursts and explosions in 'failed supernovae'
Using a two-dimensional hydrodynamics code (PROMETHEUS), we explore the continued evolution of rotating helium stars, Mα 10 M☉, in which iron-core collapse does not produce a successful outgoingExpand
...
1
2
3
4
5
...