MAGNETOROTATIONAL CORE-COLLAPSE SUPERNOVAE IN THREE DIMENSIONS

By P. Mösta, S. Richers, Christian D. Ott, Roland Haas, A. Piro, K. Boydstun, E. Abdikamalov, Christian Reisswig, Erik Schnetter. 2014

159 citations recorded by the source corpus.

We present results of new three-dimensional (3D) general-relativistic magnetohydrodynamic simulations of rapidly rotating strongly magnetized core collapse. These simulations are the first of their kind and include a microphysical finite-temperature equation of state and a leakage scheme that captures the overall energetics and lepton number exchange due to postbounce neutrino emission. Our results show that the 3D dynamics of magnetorotational core-collapse supernovae are fundamentally different from what was anticipated on the basis of previous simulations in axisymmetry (2D). A strong bipolar jet that develops in a simulation constrained to 2D is crippled by a spiral instability and fizzles in full 3D. While multiple (magneto-)hydrodynamic instabilities may be present, our analysis suggests that the jet is disrupted by an m = 1 kink instability of the ultra-strong toroidal field near the rotation axis. Instead of an axially symmetric jet, a completely new, previously unreported flow structure develops. Highly magnetized spiral plasma funnels expelled from the core push out the shock in polar regions, creating wide secularly expanding lobes. We observe no runaway explosion by the end of the full 3D simulation 185 ms after bounce. At this time, the lobes have reached maximum radii of ∼900 km.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/01d9cd62b53fa526eddc150dcba9d087302d1f7c

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Citations in the corpus

The Status of Multi-Dimensional Core-Collapse Supernova Models (2016, background): “…rotation profile.10 For very rapid rotation, other explosion mechanisms also become feasible, such as the magnetorotational mechanism (Akiyama et al. 2003; Burrows et al. 2007b; Winteler et al. 2012; Mösta et al. 2014), or explosions driven by the low-T/W spiral instability (Takiwaki et al. 2016).”
NEUTRINO-DRIVEN WINDS IN THE AFTERMATH OF A NEUTRON STAR MERGER: NUCLEOSYNTHESIS AND ELECTROMAGNETIC TRANSIENTS (2015, background): “…r-process (Arcones et al. 2007; Hüdepohl et al. 2010; Roberts et al. 2010; Fischer et al. 2010; Arcones & Montes 2011; Arcones & Thielemann 2013), though some rare supernovae may plausibly contribute (Fujimoto et al. 2006, 2008; Winteler et al. 2012; Mösta et al. 2014; Nishimura et al. 2015).”
Relativistic MHD simulations of core-collapse GRB jets: 3D instabilities and magnetic dissipation (2015, background): “In the core collapse of a massive star, heavily mass-loaded jets, which are produced by the rotation of a protoneutron star (Burrows et al. 2007), were found to be so strongly unstable to the kink instability that they were unable to penetrate the star (Mösta et al. 2014).”
The diversity of transients from magnetar birth in core collapse supernovae (2015, background): “It remains uncertain whether such a strong, ordered magnetic field is maintained in the face of non-axisymmetric instabilities (Begelman 1998; Porth et al. 2013, Mösta et al. 2014).”
Production of the entire range of r-process nuclides by black hole accretion disc outflows from neutron star mergers (2016, background): “However, current simulations of MHDpowered supernova explosions need further improvements, especially considering the role of instabilities on the jet structure which manifest in three dimensions (Mösta et al. 2014).”
Origin of the heaviest elements: The rapid neutron-capture process (2019, background): “Subsequent general relativistic simulations in 3D-MHD (Mösta et al., 2014), involving a 25 M progenitor with an initial magnetic field of 10 G, led in the early phase to jet formation, but experienced afterwards a kink instability,”
THE r-PROCESS NUCLEOSYNTHESIS IN THE VARIOUS JET-LIKE EXPLOSIONS OF MAGNETOROTATIONAL CORE-COLLAPSE SUPERNOVAE (2015, methodology): “More recent 3D-MHD simulations in the general relativistic framework (Mösta et al. 2014), involving a 25M⊙ progenitor with initial magnetic fields of 1012 G, initially lead to jet formation, which afterwards experiences a kink instability and deforms the jet-like feature.”
Neutrino-driven winds from neutron star merger remnants (2014, background): “A possible exception, though, may be magnetically driven explosions of rapidly rotating stars (Winteler et al. 2012; Mösta et al. 2014).”
The Intermediate r-process in Core-collapse Supernovae Driven by the Magneto-rotational Instability (2016, background): “…so-called magneto-rotational supernovae (MR-SNe), are a promising mechanism for several high-energy astronomical phenomena, e.g. magnetar formation, gravitational waves and hypernovae and gamma-ray bursts (e.g. Yamada & Sawai 2004; Shibata et al. 2006; Takiwaki et al. 2009; Mösta et al. 2014).”
THE DEVELOPMENT OF EXPLOSIONS IN AXISYMMETRIC AB INITIO CORE-COLLAPSE SUPERNOVA SIMULATIONS OF 12–25 M ⊙ ?> STARS (2012, methodology): “Fully general relativistic simulations with reduced neutrino physics (a leakage scheme for neutrino transport with a reduced set of neutrino interactions), have been also performed using the ZELMANI code (Ott et al. 2013; Mösta et al. 2014).”
Pulsational Pair-instability Supernovae (2016, background): “…& Wilson 1970; Meier et al. 1976; Müller & Hillebrandt 1979; Akiyama et al. 2003; Ardeljan et al. 2005; Burrows et al. 2007; Dessart et al. 2008; Takiakai & Kotake 2011; Mösta et al. 2014, 2015) universally show jets or strong bipolar outflows developing during the proto-neutron star stage.”
The overarching framework of core-collapse supernova explosions as revealed by 3D fornax simulations (2019, background): “Rapid differential rotation, on the other hand, has the potential to generate large magnetic stresses (Burrows et al. 2007; Mösta et al. 2014; Obergaulinger & Aloy 2019), with the result that strong jets can emerge.”