The Impact of Hydrodynamic Mixing on Supernova Progenitors
arXiv:astro-ph/0507104 · doi:10.1086/447769
Abstract
Recent multidimensional hydrodynamic simulations have demonstrated the importance of hydrodynamic motions in the convective boundary and radiative regions of stars to transport of energy, momentum, and composition. The impact of these processes increases with stellar mass. Stellar models which approximate this physics have been tested on several classes of observational problems. In this paper we examine the implications of the improved treatment on supernova progenitors. The improved models predict substantially different interior structures. We present pre-supernova conditions and simple explosion calculations from stellar models with and without the improved mixing treatment at 23 solar masses. The results differ substantially.
arXiv comment12 pages, 2 figures, accepted for publication in the Astrophysical Journal Letters
References in corpus (9)
- Nucleosynthesis in Massive Stars With Improved Nuclear and Stellar Physics
- Mass Limits For Black Hole Formation
- Solar Oscillations and Convection: II. Excitation of Radial Oscillations
- Two-Dimensional Hydrodynamics of Pre-Core Collapse: Oxygen Shell Burning
- Solar Oscillations and Convection: I. Formalism for Radial Oscillations
- Observational Tests and Predictive Stellar Evolution II: Non-standard Models
- Further Adventures: Oxygen Burning in a Convective Shell
- Observational Tests and Predictive Stellar Evolution
- Stellar Hydrodynamics in Radiative Regions
Cited by in corpus (22)
- Compact Remnant Mass Function: Dependence on the Explosion Mechanism and Metallicity
- The Element Abundances in Bare Planetary Nebula Central Stars and the Shell Burning in AGB Stars
- The Supernova Channel of Super-AGB Stars
- The Status of Multi-Dimensional Core-Collapse Supernova Models
- Hydrodynamics of core-collapse supernovae and their progenitors
- Multidimensional supernova simulations with approximative neutrino transport. II. Convection and the advective-acoustic cycle in the supernova core
- Constraints on the Progenitor of Cassiopeia A
- Constraints on Type Ib/c and GRB Progenitors
- Idealised hydrodynamic simulations of turbulent oxygen-burning shell convection in 4π geometry
- 3D Hydrodynamic Simulations of Carbon Burning in Massive Stars
- On the Sensitivity of Massive Star Nucleosynthesis and Evolution to Solar Abundances and to Uncertainties in Helium Burning Reaction Rates
- Hydrodynamic simulations of He-shell flash convection
- Anelastic and Compressible Simulations of Stellar Oxygen Burning
- Late-Time Convection in the Collapse of a 23 Solar Mass Star
- Uncertainties in Supernova Yields I: 1D Explosions
- Nucleosynthesis-relevant conditions in neutrino-driven supernova outflows. II. The reverse shock in two-dimensional simulations
- A Case Study of Small Scale Structure Formation in 3D Supernova Simulations
- Convective boundary mixing in a post-He core burning massive star model
- Can Stellar Mixing Explain the Lack of Type Ib Supernovae in Long-Duration GRBs?
- Nuclear Statistical Equilibrium neutrino spectrum
- 3D1D hydro-nucleosynthesis simulations. I. Advective-reactive post-processing method and its application to H ingestion into He-shell flash convection in rapidly accreting white dwarfs
- Testing a one-dimensional prescription of dynamical shear mixing with a two-dimensional hydrodynamic simulation