Magnetorotational Core-Collapse Supernovae in Three Dimensions

Mösta, Philipp; Richers, Sherwood; Ott, Christian D.; Haas, Roland; Piro, Anthony L.; Boydstun, K.; Abdikamalov, Ernazar; Reisswig, Christian; Schnetter, Erik

doi:10.1088/2041-8205/785/2/l29

Cited by 267 publications

(319 citation statements)

References 44 publications

Supporting

Mentioning

300

Contrasting

Unclassified

Order By: Relevance

“…A fraction (PJet−SN ) of high mass stars end their life as a "magneto-rotationally driven supernova" or magnetar, forming in the center a highly magnetized neutron star (with fields of the order 10 15 Gauss) and ejecting r-process matter along the poles of the rotation axis (Fujimoto et al 2006Winteler et al 2012, Mösta et al 2014). r-process simulations for such events were first undertaken in 3D by Winteler et al (2012).…”

Section: Magnetorotationally Driven Supernovae (Jet-sne)mentioning

confidence: 99%

Galactic evolution of rapid neutron capture process abundances: the inhomogeneous approach

Wehmeyer¹,

Pignatari²,

Thielemann³

2015

Mon. Not. R. Astron. Soc.

176

203

View full text Add to dashboard Cite

For the origin of heavy r-process elements, different sources have been proposed, e.g., core-collapse supernovae or neutron star mergers. Old metal-poor stars carry the signature of the astrophysical source(s). Among the elements dominantly made by the r-process, europium (Eu) is relatively easy to observe. In this work we simulate the evolution of europium in our galaxy with the inhomogeneous chemical evolution model 'ICE', and compare our results with spectroscopic observations. We test the most important parameters affecting the chemical evolution of Eu: (a) for neutron star mergers the coalescence time scale of the merger (t coal ) and the probability to experience a neutron star merger event after two supernova explosions occurred and formed a double neutron star system (P NSM ) and (b) for the sub-class of magneto-rotationally driven supernovae ("Jet-SNe"), their occurrence rate compared to standard supernovae (P Jet−SN ). We find that the observed [Eu/Fe] pattern in the galaxy can be reproduced by a combination of neutron star mergers and magneto-rotationally driven supernovae as r-process sources. While neutron star mergers alone seem to set in at too high metallicities, Jet-SNe provide a cure for this deficiency at low metallicities. Furthermore, we confirm that local inhomogeneities can explain the observed large spread in the europium abundances at low metallicities. We also predict the evolution of [O/Fe] to test whether the spread in α-elements for inhomogeneous models agrees with observations and whether this provides constraints on supernova explosion models and their nucleosynthesis.

show abstract

Section: Magnetorotationally Driven Supernovae (Jet-sne)mentioning

confidence: 99%

Galactic evolution of rapid neutron capture process abundances: the inhomogeneous approach

Wehmeyer¹,

Pignatari²,

Thielemann³

2015

Mon. Not. R. Astron. Soc.

176

203

View full text Add to dashboard Cite

show abstract

“…Takiwaki et al (2012Takiwaki et al ( , 2014 also report 3D Newtonian simulations using Zeus +IDSA. Fully general relativistic simulations with reduced neutrino physics (a leakage scheme for neutrino transport with a reduced set of neutrino interactions)have also beenper-formed using the ZELMANI code (Ott et al 2013;Mösta et al 2014).…”

Section: Introductionmentioning

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

View full text Add to dashboard Cite

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.

show abstract

“…However, it cannot deliver the explosion energies seen in some extreme CCSNe (hypernovae). Another mechanism is most likely to be at work in these events, possibly relying on rotation and magnetic fields (e.g., Burrows et al 2007;Mösta et al 2014bMösta et al , 2015.…”

Section: Introductionmentioning

confidence: 99%

General-Relativistic Three-Dimensional Multi-Group Neutrino Radiation-Hydrodynamics Simulations of Core-Collapse Supernovae

Roberts

Ott

Haas

et al. 2016

ApJ

Self Cite

187

182

View full text Add to dashboard Cite

We report on a set of long-term general-relativistic three-dimensional (3D) multi-group (energy-dependent) neutrino radiation-hydrodynamics simulations of core-collapse supernovae. We employ a full 3D two-moment scheme with the local M1 closure, three neutrino species, and 12 energy groups per species. With this, we follow the post-core-bounce evolution of the core of a nonrotating - M 27 progenitor in full unconstrained 3D and in octant symmetry for 380 ms. We find the development of an asymmetric runaway explosion in our unconstrained simulation. We test the resolution dependence of our results and, in agreement with previous work, find that low resolution artificially aids explosion and leads to an earlier runaway expansion of the shock. At low resolution, the octant and full 3D dynamics are qualitatively very similar, but at high resolution, only the full 3D simulation exhibits the onset of explosion.

show abstract

Magnetorotational Core-Collapse Supernovae in Three Dimensions

Cited by 267 publications

References 44 publications

Galactic evolution of rapid neutron capture process abundances: the inhomogeneous approach

Galactic evolution of rapid neutron capture process abundances: the inhomogeneous approach

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

General-Relativistic Three-Dimensional Multi-Group Neutrino Radiation-Hydrodynamics Simulations of Core-Collapse Supernovae

Contact Info

Product

Resources

About