Presupernova Evolution of Differentially Rotating Massive Stars Including Magnetic Fields

By Alexander Heger, Stan Woosley, H. Spruit. 2004

618 citations recorded by the source corpus.

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 a variety of classic instabilities and also by magnetic torques from fields generated by the differential rotation. We present the first stellar evolution calculations to follow the evolution of rotating massive stars including, at least approximately, all these effects, magnetic and nonmagnetic, from the zero-age main sequence until the onset of iron-core collapse. The evolution and action of the magnetic fields is as described by Spruit in 2002, and a range of uncertain parameters is explored. In general, we find that magnetic torques decrease the final rotation rate of the collapsing iron core by about a factor of 30-50 when compared with the nonmagnetic counterparts. Angular momentum in that part of the presupernova star destined to become a neutron star is an increasing function of main-sequence mass. That is, pulsars derived from more massive stars rotate faster and rotation plays a more important role in the star's explosion. The final angular momentum of the core has been determined—to within a factor of 2—by the time the star ignites carbon burning. For the lighter stars studied, around 15 M☉, we predict pulsar periods at birth near 15 ms, though a factor of 2 range is easily tolerated by the uncertainties. Several mechanisms for additional braking in a young neutron star, especially by fallback, are explored.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/f663a9230155d8275f82e96121124437ba49509a

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Rotating massive main-sequence stars - I. Grids of evolutionary models and isochrones (2011, background): “Heuristically, angular momentum transport through magnetic fields produced by the SpruitTayler dynamo, as the so far only mechanism, appears to reproduce the rotation rates of white dwarfs and neutron stars quite well (Heger et al. 2005; Suijs et al. 2008).”
Temporal and Angular Properties of Gamma-Ray Burst Jets Emerging from Massive Stars (2006, background): “This value of pressure at 1010 cm is reasonable based on numerically modeled values for stars of similar size andmass (Heger et al. 2005).”
Neutron Star Kicks by the Gravitational Tug-boat Mechanism in Asymmetric Supernova Explosions: Progenitor and Explosion Dependence (2016, background): “…unlikely explanation for the putative spin-kick alignment is the fact that in the far majority of cases stellar cores at the time of collapse do not possess the huge amount of angular momentum (with specific values in excess of ∼1016 cm2 s−1) needed for disk and jet formation (Heger et al. 2005).”
Stellar evolution with rotation - XIII. Predicted GRB rates at various Z (2005, background): “Heger et al. (2005) show that the braking by magnetic fields, which are produced by differential rotation during the evolution (see Spruit 2002) significantly reduce the discrepancy between the predicted and observed pulsar periods.”
Models of low-mass helium white dwarfs including gravitational settling, thermal and chemical diffusion, and rotational mixing (2016, background): “The mixing of angular momentum that is due to dynamo-generated magnetic fields in radiative zones is also included (Spruit 2002; Heger et al. 2005) as is the angular momentum transport due to electron viscosity (Itoh et al. 1987).”
The Supernova Gamma-Ray Burst Connection (2006, background): “However, incorporation of approximate magnetic torques (Spruit, 2002) in single stars that evolve through a red giant phase gives too little rotation for GRBs (Heger et al., 2005), though just about the right amount for pulsars (Ott et al., 2005).”
MAGNETOROTATIONALLY DRIVEN SUPERNOVAE AS THE ORIGIN OF EARLY GALAXY r-PROCESS ELEMENTS? (2012, methodology): “We employed the pre-collapse 15M⊙ model of Heger et al. (2005).”
The Gravitational Wave Signal from Core-collapse Supernovae (2018, background): “The main limitation of these papers is that fast rotating cores are not very common among CCSN progenitors (Heger et al. 2005; Woosley & Heger 2006).”
Equation-of-state dependent features in shock-oscillation modulated neutrino and gravitational-wave signals from supernovae (2008, result): “This, however, does not seem to be compatible with predictions from the latest generation of stellar evolution models for the vast majority of massive stars, which are expected to have lost most of their angular momentum before collapse (Heger et al. 2005).”
Two-Dimensional Multiangle, Multigroup Neutrino Radiation-Hydrodynamic Simulations of Postbounce Supernova Cores (2008, background): “This rotation law enforces constant angular velocity on cylindrical shells and, for sensible choices ofA, reproduces qualitatively (Ott et al. 2006b) predictions from presupernova models that include rotation in a 1D fashion (Heger et al. 2000, 2005).”
Pulsational Pair-instability Supernovae (2016, methodology): “The same metallicity (10% solar) was employed and magnetic torques were included in all models (Heger et al. 2005).”
The origin of spin in binary black holes (2019, methodology): “From observations of astro-seismology (Fuller et al. 2014; Cantiello et al. 2014), as well as neutron star and white dwarf spins (Heger et al. 2005; Suijs et al. 2008), it is known that this mechanism must be efficient (Spruit 1999, 2002; Fuller et al. 2019).”
PRE-SUPERNOVA EVOLUTION OF ROTATING SOLAR METALLICITY STARS IN THE MASS RANGE 13–120 M☉ AND THEIR EXPLOSIVE YIELDS (2012, neutral): “…and discussed by Meynet & Maeder (2000, 2003); Hirschi et al. (2004); Meynet & Maeder (2005); Decressin et al. (2007); Ekström et al. (2008); Ekström et al. (2012) and Heger et al. (2000); Heger & Langer (2000); Heger et al. (2005); Yoon & Langer (2005); Yoon et al. (2006); Brott et al. (2011).”
Binary star progenitors of long gamma-ray bursts (2007, background): “…(Petrovic et al. 2005b; Hirschi et al. 2005), only models including magnetic fields are capable of reproducing the slow spins of young Galactic neutron stars (Heger et al. 2005; Ott et al. 2006) and white dwarfs (Suijs et al. 2007), due to the magnetic coreenvelope coupling during the giant stage.”
A MODEL FOR GRAVITATIONAL WAVE EMISSION FROM NEUTRINO-DRIVEN CORE-COLLAPSE SUPERNOVAE (2009, background): “However, the rotation rates necessary for GWs with sizeable amplitudes are likely to obtain in only ∼1% of the massive star population (Heger et al. 2005; Hirschi et al. 2004; Woosley & Heger 2006; Ott et al. 2006b).”