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

  title={Presupernova Evolution of Rotating Massive Stars. I. Numerical Method and Evolution of the Internal Stellar Structure},
  author={A. Heger and N. Langer and S. Ucsc and Mpa and U. Potsdam},
  journal={The Astrophysical Journal},
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
Stellar evolution with rotation XII. Pre-supernova models
We describe the latest developments of the Geneva stellar evolution code in order to model the pre-supernova evolution of rotating massive stars. Rotating and non-rotating stellar models at solarExpand
Presupernova Evolution of Rotating Massive Stars. II. Evolution of the Surface Properties
We investigate the evolution of the surface properties of models for rotating massive stars, i.e., their luminosities, effective temperatures, surface rotational velocities, and surface abundances ofExpand
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
Presupernova evolution of differentially rotating massive stars including magnetic fields
As a massive star evolves through multiple stages of nuclear burning on its way to becoming a supernova, a complex, differentially rotating structure is set up. Angular momentum is transported by aExpand
Presupernova evolution of rotating massive stars and the rotation rate of pulsars
Rotation in massive stars has been studied on the main sequence and during helium burning for decades, but only recently have realistic numerical simulations followed the transport of angularExpand
Evolution of massive Population III stars with rotation and magnetic fields
Context. Aims. We present a new grid of massive population III (Pop III) star models including the effects of rotation on the stellar structure and chemical mixing, and magnetic torques for theExpand
The evolution of rotating very massive stars with LMC composition
Context. With growing evidence for the existence of very massive stars at subsolar metallicity, there is an increased need for corresponding stellar evolution models. Aims. We present a dense modelExpand
Evolution of single B-type stars with a large angular momentum content
Context. The Geneva Stellar Evolution Group has recently presented an extended database of rotating stellar models at three different metallicities for nine different initial rotation parameters andExpand
We have computed new stellar evolution models that include the effects of rotation and magnetic torques under different hypotheses. The goal is to test whether a single star can sustain theExpand
We present the first set of a new generation of models of massive stars with a solar composition extending between 13 and 120 M ?, computed with and without the effects of rotation. We included twoExpand


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