Three-dimensional neutrino-driven supernovae: neutron star kicks, spins, and asymmetric ejection of nucleosynthesis products

By A. Wongwathanarat, Hans-Thomas Janka, Ewald Müller. 2012

221 citations recorded by the source corpus.

We present three-dimensional (3D) simulations of supernova explosions of nonrotating stars, triggered by the delayed neutrinoheating mechanism with a suitable choice of the core-neutrino luminosity. Our results show that asymmetric mass ejection caused by hydrodynamic instabilities can accelerate the neutron star (NS) up to recoil velocities of more than 700 km s 1 by the “gravitational tug-boat mechanism”, which is su cient to explain most observed pulsar space velocities. The associated NS spin periods for our nonrotating progenitors are about 100 ms to 8000 ms without any obvious correlation between spin and kick magnitudes or directions. This suggests that faster spins and a possible spin-kick alignment might require angular momentum in the progenitor core prior to collapse. Our simulations for the first time demonstrate a clear correlation between the size of the NS kick and anisotropic production and distribution of heavy elements created by explosive burning behind the shock. In the case of large pulsar kicks the explosion is significantly stronger opposite to the kick vector. Therefore the bulk of the explosively fused iron-group elements, in particular nickel, is ejected mostly in large clumps against the kick direction. This contrasts with the case of low recoil velocity, where the nickel-rich lumps are more isotropically distributed. Explosively produced intermediate-mass nuclei heavier than 28 Si (like 40 Ca and 44 Ti) also exhibit a significant enhancement in the hemisphere opposite to the direction of fast NS motion, while the distribution of 12 C, 16 O, and 20 Ne is not a ected, and that of 24 Mg only marginally. Mapping the spatial distribution of the heavy elements in supernova remnants with identified pulsar motion may o er an important diagnostic test of the kick mechanism. Di erent from kick scenarios based on anisotropic neutrino emission, our hydrodynamical acceleration model predicts enhanced ejection of iron-group elements and of their nuclear precursors in the direction opposite to the NS recoil.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/a4f53b3c481db374a23f6f3b103837c1989c3f59

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Citations in the corpus

THE DEVELOPMENT OF EXPLOSIONS IN AXISYMMETRIC AB INITIO CORE-COLLAPSE SUPERNOVA SIMULATIONS OF 12–25 M ⊙ ?> STARS (2012, methodology): “The second method involves computing the acceleration of the proto-NS by summing up all the forces acting upon it, and integrating with respect to time to compute the velocity (Scheck et al. 2006; Nordhaus et al. 2010; Wongwathanarat et al. 2010, 2013).”
Three-dimensional simulations of core-collapse supernovae: from shock revival to shock breakout (2014, methodology): “The simulations presented here are initialized from 3D neutrinodriven explosion models (see Table 1) discussed in our previous studies (Wongwathanarat et al. 2010b, 2013), which covered the evolution from 11–15 ms to 1.1–1.4 s after core bounce.”
SELF-SUSTAINED ASYMMETRY OF LEPTON-NUMBER EMISSION: A NEW PHENOMENON DURING THE SUPERNOVA SHOCK-ACCRETION PHASE IN THREE DIMENSIONS (2014, background): “…dipole survives for seconds, however, the estimated recoil velocity is dwarfed by those that can typically be expected from the “gravitational tug-boat mechanism” associated with the anisotropic ejection of matter in 3D simulations of SN explosions (Wongwathanarat et al. 2010, 2013).”
Massive runaway and walkaway stars (2018, methodology): “Such kicks are expected either from asymmetries in the explosion and/or the neutrino emission (Shklovskii 1970; Wongwathanarat et al. 2013; Janka 2013, 2017), and they determine which systems disrupt and eject the companion star and which systems remain bound and thus have a potential as future…”
SASI ACTIVITY IN THREE-DIMENSIONAL NEUTRINO-HYDRODYNAMICS SIMULATIONS OF SUPERNOVA CORES (2013, methodology): “…largescale anisotropies in the ejecta may yield a natural explanation for the observed high kick velocities of young pulsars (Janka & Müller 1994; Herant 1995; Burrows & Hayes 1996; Scheck et al. 2004, 2006; Wongwathanarat et al. 2010b; Nordhaus et al. 2010a, 2012; Wongwathanarat et al. 2012).”
Three-dimensional simulations of neutrino-driven core-collapse supernovae from low-mass single and binary star progenitors (2018, methodology): “As in parameterised 3D simulations (Wongwathanarat et al. 2013; Gessner & Janka 2018) we do not find any evidence for spinkick alignment.”
Ultra-stripped supernovae: progenitors and fate (2015, background): “These instabilities lead to large-scale anisotropies of the innermost SN ejecta, which interact gravitationally with the proto-NS and accelerate the nascent NS on a timescal of several seconds (e.g. Janka 2012; Wongwathanarat et al. 2013).”
A COMPARISON OF TWO- AND THREE-DIMENSIONAL NEUTRINO-HYDRODYNAMICS SIMULATIONS OF CORE-COLLAPSE SUPERNOVAE (2013, background): “A number of exciting issues also remain to be investigated, such as gravitational-wave signatures (e.g., Kotake (2013)), neutrino emission and its detectability (e.g., Lund et al. (2012)), and the possi- bility of 3D SASI flows generating pulsar kicks and spins (e.g., Wongwathanarat et al. (2013)).”