Radiation hydrodynamics with neutrinos

Rampp, Markus; Janka, Hans‐Thomas

doi:10.1051/0004-6361:20021398

Cited by 392 publications

(569 citation statements)

References 84 publications

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“…In our implementation of these processes, we follow Rampp & Janka (2002). Due to their stiffness, we solve these source terms implicitly and split them off from the other parts of the conservation equations by an operator-split step.…”

Section: Physical Model and Numerical Methodsmentioning

confidence: 99%

Magnetic field amplification and magnetically supported explosions of collapsing, non-rotating stellar cores

Obergaulinger¹,

Janka²,

Aloy³

2014

Monthly Notices of the Royal Astronomical Society

104

117

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We study the amplification of magnetic fields in the collapse and the post-bounce evolution of the core of a non-rotating star of 15 M in axisymmetry. To this end, we solve the coupled equations of magnetohydrodynamics and neutrino transport in the two-moment approximation. The pre-collapse magnetic field is strongly amplified by compression in the infall. Initial fields of the order of 10 10 G translate into proto-neutron star fields similar to the ones observed in pulsars, while stronger initial fields yield magnetar-like final field strengths. After core bounce, the field is advected through the hydrodynamically unstable neutrino-heating layer, where non-radial flows due to convection and the standing accretion shock instability amplify the field further. Consequently, the resulting amplification factor of order five is the result of the number of small-eddy turnovers taking place within the time scale of advection through the post-shock layer. Due to this limit, most of our models do not reach equipartition between kinetic and magnetic energy and, consequently, evolve similarly to the non-magnetic case, exploding after about 800 ms when a single or few highentropy bubbles persist over several dynamical time scales. In the model with the strongest initial field we studied, 10 12 G, for which equipartition between flow and field is achieved, the magnetic tension favours a much earlier development of such long-lived high-entropy bubbles and enforces a fairly ordered large-scale flow pattern. Consequently, this model, after exhibiting very regular shock oscillations, explodes much earlier than non-magnetic ones.

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Section: Physical Model and Numerical Methodsmentioning

confidence: 99%

Magnetic field amplification and magnetically supported explosions of collapsing, non-rotating stellar cores

Obergaulinger¹,

Janka²,

Aloy³

2014

Monthly Notices of the Royal Astronomical Society

104

117

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“…Another difference is our use of the revised Cooperstein EoS in the region between the neutrinosphere and the shock. The PROMETHEUS-VERTEX code (Rampp & Janka 2002;Marek et al 2006), with Newtonian hydrodynamics and the same psuedo-Newtonian (spherical GR corrections to Newtonian) gravity treatment implemented in CHIMERA, was used by Buras et al (2006aBuras et al ( , 2006b and Marek & Janka (2009) to evolve, in axisymmetry, the 15 M  progenitor s15s7b2 of Woosley & Weaver (1995). Müller et al (2012b) also evolved s15s7b2 using the COCONUT-VERTEX code , which employes the conformal flatness GR approximation rather than a pseudo-Newtonian approximation to the hydrodynamics, gravity, and RbR transport.…”

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

203

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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“…For this reason we have performed a Boltzmann transport simulation coupled with a full hydrodynamics code (Rampp & Janka 2002) for the 15 M progenitor model s15s7b2 (S. E. Woosley 1997, private communication;Woosley & Weaver 1995).…”

Section: Hydrodynamic Simulation With Boltzmann Transportmentioning

confidence: 99%

“…Neutrino-medium interactions for all relevant processes are implemented, notably nucleon bremsstrahlung, as described by Rampp & Janka (2002). Note, however, that nucleon recoils are not taken into account in the results shown for the baseline simulation (Figs.…”

Section: Hydrodynamic Simulation With Boltzmann Transportmentioning

confidence: 99%

“…However, with the advent of numerical Boltzmann solvers for the neutrino transport (Mezzacappa & Bruenn 1993;Mezzacappa & Messer 1999;Yamada, Janka, & Suzuki 1999;Burrows et al 2000;Rampp & Janka 2002) and their application to the postbounce phase of stellar core-collapse models (Rampp & Janka 2000;Mezzacappa et al 2001;Liebendö rfer et al 2001), a new level of accuracy has been achieved. Evidently, it is desirable that in consistent state-of-the-art simulations the uncertainties not be dominated by overly crude approximations of the microphysics that governs the neutrino interactions.…”

Section: Introductionmentioning

confidence: 99%

See 1 more Smart Citation

Electron Neutrino Pair Annihilation: A New Source for Muon and Tau Neutrinos in Supernovae

Buras

Janka

Keil³

et al. 2003

ApJ

132

179

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We show that in a supernova core the annihilation process e e ! l; l; is always more important than the traditional reaction e þ e À ! l; l; as a source for muon and tau neutrino pairs. We study the impact of the new process by means of a Monte Carlo transport code with a static stellar background model and by means of a self-consistent hydrodynamic simulation with Boltzmann neutrino transport. Nucleon

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Radiation hydrodynamics with neutrinos

Cited by 392 publications

References 84 publications

Magnetic field amplification and magnetically supported explosions of collapsing, non-rotating stellar cores

Magnetic field amplification and magnetically supported explosions of collapsing, non-rotating stellar cores

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

Electron Neutrino Pair Annihilation: A New Source for Muon and Tau Neutrinos in Supernovae

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