REVIEW 9 cited by
Presupernova Evolution of Differentially Rotating Massive Stars Including Magnetic Fields
Not yet reviewed by Pith; the record is open.
This paper has not been read by Pith yet. Machine review is queued; the pith claim, tier, and objections will appear here once it completes.
SPECIMEN: schema-true, not a live event
T0 review · schema-true
One-sentence machine reading of the paper's core claim.
pith:XXXXXXXX · record.json · timestamp
Signed reviews
read the original abstract
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 non-magnetic, 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 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 to 50 when compared with the non-magnetic 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 will rotate faster and rotation will play a more dominant role in the star's explosion. The final angular momentum of the core is determined - to within a factor of two - by the time the star ignites carbon burning. For the lighter stars studied, around 15 solar masses, we predict pulsar periods at birth near 15 ms, though a factor of two range is easily tolerated by the uncertainties. Several mechanisms for additional braking in a young neutron star, especially by fall back, are also explored.
Forward citations
Cited by 9 Pith papers
-
3D simulations of a complete convective silicon shell burning phase
A 3D simulation of a convective silicon-burning shell in a 14 solar mass star burns out about 800 s earlier than a 1D MESA model, suggesting weaker convective boundary mixing and a convective-reactive energy profile.
-
Neutron star-companion interaction in core collapse supernovae. Population synthesis based on detailed binary evolution models
Population synthesis from binary evolution models predicts periodic neutron star-companion interactions in more than half of surviving hydrogen-poor core-collapse supernovae, with periods peaking at 20-50 days and las...
-
Astrophysics and cosmology with a decihertz gravitational-wave detector: TianGO
A decihertz space gravitational-wave detector paired with a ground network would localize compact binary mergers far more precisely than the ground network alone, supporting standard-siren cosmology, early warning, an...
-
High Power Accretion in Massive Binary Systems and the Impact of Metallicity
Higher-metallicity massive stars show larger accretion-driven luminosity increases despite being more extended, and flip to a cool inflated state at lower accretion rates than low-metallicity stars.
-
Analysis and simulations of binary black hole merger spins -- the question of spin-axis tossing at black hole formation
Simulated effective-spin distributions match LVK O1-O3 data for isolated binaries only when black hole spin axes are tossed at formation, or if roughly 72% of mergers have a dynamical origin.
-
Toward More Realistic Machine-Learning Inference of the Dense-Matter Equation of State from Supernova Gravitational Waves
Using a linear SVM, EOS classification from bounce gravitational waves remains robust to real noise, progenitor diversity, and bounce-time uncertainty in the frequency domain, but collapses in the time domain under ti...
-
Parameter Estimation Horizon of Core-Collapse Supernovae with a Network of Gravitational-Wave Detectors
A CNN can recover supernova peak frequency out to about 30 kpc and rotation/amplitude out to 200-250 kpc with current networks, extending to roughly 300 kpc and 2-2.5 Mpc with third-generation detectors.
-
Dynamical formation of long-period exoplanets systems in evolving binary stars
MESA+REBOUND simulations show that stellar mass loss in a wide binary destabilizes S-type multi-planet systems and pushes surviving giants to long-period orbits.
-
Comparative Study of Two Luminous Red Novae I. Progenitor Modeling and Dust Formation
Binary evolution modeling constrains donor masses of 14-23 solar masses for two luminous red novae and shows dust masses are 1-5 orders of magnitude below total ejected envelope masses.
Discussion (0). Continue with ORCID to comment.