Simulating Radiating and Magnetized Flows in Multiple Dimensions with ZEUS‐MP

Hayes, John C.; Norman, Michael L.; Fiedler, Robert; Bordner, James; Li, Pak Shing; Clark, S. E.; ud‐Doula, Asif; Low, Mordecai–Mark Mac

doi:10.1086/504594

Cited by 321 publications

(334 citation statements)

References 53 publications

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“…All the simulations presented here are done with the ZEUS MP code (Hayes et al 2006). This is a three dimensional Newtonian magneto-hydrodynamics code, which solves the Euler equations on a staggered mesh grid.…”

Section: Methodsmentioning

confidence: 99%

The hydrodynamics of the supernova remnant Cassiopeia A

Veelen

Langer

Vink

et al. 2009

A&A

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Aims. There are large differences in the proposed progenitor models for the Cas A SNR. One of these differences is the presence or absence of a Wolf-Rayet (WR) phase of the progenitor star. The mass loss history of the progenitor star strongly affects the shape of the Supernova remnant (SNR). In this paper we investigate whether the progenitor star of Cas A had a WR phase or not and how long it may have lasted.Methods. We performed two-dimensional multi-species hydrodynamical simulations of the CSM around the progenitor star for several WR life times, each followed by the interaction of the supernova ejecta with the CSM. We then looked at the influence of the length of the WR phase and compared the results of the simulations with the observations of Cas A. Results. The difference in the structure of the CSM, for models with different WR life times, has a strong impact on the resulting SNR. With an increasing WR life time the reverse shock velocity of the SNR decreases and the range of observed velocities in the shocked material increases. Furthermore, if a WR phase occurs, the remainders of the WR shell will be visible in the resulting SNR. Conclusions. Comparing our results with the observations suggests that the progenitor star of Cas A did not have a WR phase. We also find that the quasi-stationary flocculi (QSF) in Cas A are not consistent with the clumps from a WR shell that have been shocked and accelerated by the interaction with the SN ejecta. We can also conclude that for a SN explosion taking place in a CSM that is shaped by the wind during a short (≤ 15000 yr) WR phase, the clumps from the WR shell will be visible inside the SNR.

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Section: Methodsmentioning

confidence: 99%

The hydrodynamics of the supernova remnant Cassiopeia A

Veelen

Langer

Vink

et al. 2009

A&A

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“…A fourth group has used a version of the Zeus-MP code (Hayes et al 2006;Iwakami et al 2008Iwakami et al , 2009a for hydrodynamics and the IDSA scheme for neutrino transport (Liebendörfer et al 2009), which we will refer to as "Zeus +IDSA." Zeus+IDSA is fully Newtonian and the transport omits inelastic (energy exchanging) scattering in favor of the elastic versions.…”

Section: Other Axisymmetric Simulationsmentioning

confidence: 99%

The Development of Explosions in Axisymmetric Ab Initio Core-Collapse Supernova Simulations of 12–25 Stars

Bruenn

Lentz

Hix

et al. 2016

ApJ

204

300

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We present four ab initio axisymmetric core-collapse supernova simulations initiated from 12, 15, 20, and 25 M  zero-age main sequence progenitors. All of the simulations yield explosions and havebeen evolved for at least 1.2 s after core bounce and 1 s after material first becomes unbound. These simulations were computed with our CHIMERA code employing RbR spectral neutrino transport, special and general relativistic transport effects, and state-of-the-art neutrino interactions. Continuing the evolution beyond 1 s after core bounce allows the explosions to develop more fully and the processes involved in powering the explosions to become more clearly evident. We compute explosion energy estimates, including the negative gravitational binding energy of the stellar envelope outside the expanding shock, of 0.34, 0.88, 0.38, and 0.70 Bethe (B≡10 51 erg) and increasing at 0.03, 0.15, 0.19, and 0.52 B s 1 -, respectively, for the 12, 15, 20, and 25 M  models at the endpoint of this report. We examine the growth of the explosion energy in our models through detailed analyses of the energy sources and flows. We discuss how the explosion energies may be subject to stochastic variations as exemplfied by the effect of the explosion geometry of the 20 M  model in reducing its explosion energy. We compute the proto-neutron star masses and kick velocities. We compare our results for the explosion energies and ejected Ni 56 masses against some observational standards despite the large error bars in both models and observations.

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“…We employ the equation of state (EOS) by Lattimer & Swesty (1991) with a compressibility modulus of K = 220 MeV (LS220). For the calculations presented here, self-gravity is computed by a Newtonian monopole approximation and our code is updated, from the ZEUS-MP (Hayes et al 2006) code as was used in Takiwaki et al (2014), to use high-resolution shock capturing scheme with an approximate Riemann solver of Einfeldt (1988) for more details).…”

Section: Numerical Schemementioning

confidence: 99%

Systematic features of axisymmetric neutrino-driven core-collapse supernova models in multiple progenitors

Nakamura

Takiwaki

Kuroda

et al. 2015

Publications of the Astronomical Society of Japan

128

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We present an overview of two-dimensional (2D) core-collapse supernova simulations employing neutrino transport scheme by the isotropic diffusion source approximation. We study 101 solar-metallicity, 247 ultra metal-poor, and 30 zero-metal progenitors covering zero-age main sequence mass from 10.8 M ⊙ to 75.0 M ⊙ . Using the 378 progenitors in total, we systematically investigate how the differences in the structures of these multiple progenitors impact the hydrodynamics evolution. By following a long-term evolution over 1.0 s after bounce, most of the computed models exhibit neutrino-driven revival of the stalled bounce shock at ∼ 200 -800 ms postbounce, leading to the possibility of explosion. Pushing the boundaries of expectations in previous one-dimensional (1D) studies, our results confirm that the compactness parameter ξ that characterizes the structure of the progenitors is also a key in 2D to diagnose the properties of neutrinodriven explosions. Models with high ξ undergo high ram pressure from the accreting matter onto the stalled shock, which affects the subsequent evolution of the shock expansion and the mass of the protoneutron star under the influence of neutrino-driven convection and the standing accretion-shock instability. We show that the accretion luminosity becomes higher for models with high ξ, which makes the growth rate of the diagnostic explosion energy higher and the synthesized nickel mass bigger. We find that these explosion characteristics tend to show a monotonic increase as a function of the compactness parameter ξ.

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Simulating Radiating and Magnetized Flows in Multiple Dimensions with ZEUS‐MP

Cited by 321 publications

References 53 publications

The hydrodynamics of the supernova remnant Cassiopeia A

The hydrodynamics of the supernova remnant Cassiopeia A

The Development of Explosions in Axisymmetric Ab Initio Core-Collapse Supernova Simulations of 12–25 Stars

Systematic features of axisymmetric neutrino-driven core-collapse supernova models in multiple progenitors

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