The physics of core-collapse supernovae

@article{Woosley2005ThePO,
  title={The physics of core-collapse supernovae},
  author={S. E. Woosley and Thomas Janka},
  journal={Nature Physics},
  year={2005},
  volume={1},
  pages={147-154}
}
Supernovae are nature’s grandest explosions and an astrophysical laboratory in which unique conditions exist that are not achievable on Earth. They are also the furnaces in which most of the elements heavier than carbon have been forged. Scientists have argued for decades about the physical mechanism responsible for these explosions. It is clear that the ultimate energy source is gravity, but the relative roles of neutrinos, fluid instabilities, rotation and magnetic fields continue to be… 

Core-collapse supernova explosion theory

The delayed neutrino-heating mechanism is emerging as the key driver of supernova explosions, but there remain many issues to address, such as the chaos of the involved dynamics.

Explosion Mechanisms of Core-Collapse Supernovae

Supernova theory, numerical and analytic, has made remarkable progress in the past decade. This progress was made possible by more sophisticated simulation tools, especially for neutrino transport,

Neutrino signatures of near-critical supernova outflows

In a core-collapse supernova, after the explosion is launched, neutrino heating above the protoneutron star creates an outflow of matter. This outflow has been extensively investigated as a

Supernovae at the cosmic dawn

Modern cosmological simulations predict that the first generation of stars formed with a mass scale around 100 solar masses about 300-400 million years after the Big Bang. When the first stars

3 Astrophysical Axion Bounds

Axion emission by hot and dense plasmas is a new energy-loss channel for stars. Observable consequences include a modification of the solar sound-speed profile, an increase of the solar neutrino

The e-ASTROGAM space mission: a major step forward for supernova physics

Abstract e-ASTROGAM is a gamma-ray observatory operating in a broad energy range, 0.15 MeV – 3 GeV, recently proposed as the M5 Medium-size mission of the European Space Agency. It has the potential

Gravitational waves from 3D MHD core-collapse supernova simulations with neutrino transport

Core-collapse supernovae (CCSNe) are among the most energetic explosions in the universe, liberating the prodigious amount of ~ 1053 erg, the binding energy of their compact remnants, neutron stars

Axion Bounds

Axion emission by hot and dense plasmas is a new energy-loss channel for stars. Observational consequences include a modification of the solar sound-speed profile, an increase of the solar neutrino

The origin of the elements as seen through supernova remnants

Supernovae are the main sites of heavy element production in galaxies. Observing their remnants at a relatively early stage of a few hundred years after the explosion provides a direct view of the

Reaction data in helium and carbon burning

Nuclear fusion reactions play a key role in the understanding of energy production, nucleosynthesis of the elements in stars and the evolution of massive stars. Therefore, the direct determination of
...

References

SHOWING 1-10 OF 64 REFERENCES

On the nature of core-collapse supernova explosions

We investigate in this paper the core-collapse supernova explosion mechanism in both one and two dimensions. We verify the usefulness of neutrino-driven overturn (``convection'') between the shock

Supernova mechanisms. [SN 1987a]

Supernovae of Type II occur at the end of the evolution of massive stars. The phenomenon begins when the iron core of the star exceeds a Chandrasekhar mass. The collapse of that core under gravity is

Pulsar recoil by large-scale anisotropies in supernova explosions.

It is shown that low-mode (l=1,2) convection can develop from random seed perturbations behind the shock, requiring the core luminosity to vary slowly with time, in contrast to the burstlike exponential decay assumed in previous work.

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⊙),

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 outgoing

The r-process and neutrino-heated supernova ejecta

As a neutron star is formed by the collapse of the iron core of a massive star, its Kelvin-Helmholtz evolution is characterized by the release of gravitational binding energy as neutrinos. The

Nucleosynthesis in Neutrino-Driven Winds. I. The Physical Conditions

During the first 20 s of its life, the enormous neutrino luminosity of a neutron star drives appreciable mass loss from its surface. Previous investigations have shown that this neutrino-driven wind

Type II supernovae in 12Mcirdot and 15Mcirdot stars: The equation of state and general relativity.

We present results of hydrodynamic calculations of iron core collapse and subsequent shock propagation using the 12M/sub c/irdot and 15M/sub c/irdot initial models of Woosley and Weaver. A softening

The Collapse of Rotating Massive Stars in Three Dimensions

Most simulations of the core collapse of massive stars have focused on the collapse of spherically symmetric objects. If these stars are rotating, this symmetry is broken, opening up a number of
...