Multidimensional supernova simulations with approximative neutrino transport. I. Neutron star kicks and the anisotropy of neutrino-driven explosions in two spatial dimensions

By L. Scheck, K. Kifonidis, Hans-Thomas Janka, E. Mueller. 2006

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We study hydrodynamic instabilities during the first seconds of core-collapse supernovae by means of 2D simulations with approximative neutrino transport and boundary conditions that parameterize the effects of the contracting neutron star and allow us to obtain sufficiently strong neutrino heating and, hence, neutrino-driven explosions. Confirming more idealised studies, as well as supernova simulations with spectral transport, we find that random seed perturbations can grow by hydrodynamic instabilities to a globally asymmetric mass distribution in the region between the nascent neutron star and the accretion shock, leading to a dominance of dipole ($l=1$) and quadrupole ($l=2$) modes in the explosion ejecta, provided the onset of the supernova explosion is sufficiently slower than the growth time scale of the low-mode instability. By gravitational and hydrodynamic forces, the anisotropic mass distribution causes an acceleration of the nascent neutron star, which lasts for several seconds and can propel the neutron star to velocities of more than 1000 km s -1 . Because the explosion anisotropies develop chaotically and change by small differences in the fluid flow, the magnitude of the kick varies stochastically. No systematic dependence of the average neutron star velocity on the explosion energy or the properties of the considered progenitors is found. Instead, the anisotropy of the mass ejection, and hence of the kick, seems to increase when the nascent neutron star contracts more quickly, and thus low-mode instabilities can grow more rapidly. Our more than 70 models separate into two groups, one with high and the other with low neutron star velocities and accelerations after one second of post-bounce evolution, depending on whether the $l=1$ mode is dominant in the ejecta or not. This leads to a bimodality of the distribution when the neutron star velocities are extrapolated to their terminal values. Establishing a link to the measured distribution of pulsar velocities, however, requires a much larger set of calculations and ultimately 3D modelling.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/bddb43a9c489282769306625fe8a927d7e2dc181

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Citations in the corpus

Features of the Acoustic Mechanism of Core-Collapse Supernova Explosions (2006, methodology): “This is a firm prediction of the model (see also Scheck et al. 2004,2006).”
Multiple physical elements to determine the gravitational-wave signatures of core-collapse supernovae (2011, background): “words in (...) for making the meaning of the sentence complete. 5except for 8 − 9M⊙ stars (e.g., [51]). 3 (e.g., [52, 53, 54, 55, 56]) as well as the Standing-Accretion-Shock-Instability (SASI, e.g., [57, 58, 59, 60, 61, 62, 63, 64, 65, 66, 67, 68] see references therein) can help the onset of the n”
On the nature of supernovae Ib and Ic (2012, background): “…28 July 2018 as in the collapsar model (Woosley 1993), an intrinsic large-scale asymmetry of the shock in an explosion through the neutrino mechanism (Scheck et al. 2006; Marek & Janka 2009) or the magnetorotational mechanism (LeBlanc & Wilson 1970; Bisnovatyi-Kogan, Popov & Samokhin 1976;…”
Neutron Star Kicks by the Gravitational Tug-boat Mechanism in Asymmetric Supernova Explosions: Progenitor and Explosion Dependence (2016, methodology): “…explosions of electroncapture SN models in 2D and 3D between ∼0.2 × 1050 erg and ∼1.7×1050 erg, Gessner (2014) obtained values of αej ten times lower than Scheck et al. (2006) (i.e., up to about 0.036) and NS kick velocities of at most a few km s−1 (the maximum kick velocities were around 6 km…”
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).”
GENERAL-RELATIVISTIC SIMULATIONS OF THREE-DIMENSIONAL CORE-COLLAPSE SUPERNOVAE (2012, background): “…to larger average shock radii, increase the dwell time of material in the gain region, may lead to secondary shocks, and are thus generally aiding the explosion mechanism (Ohnishi et al. 2006; Scheck et al. 2006; Murphy & Burrows 2008; Ott et al. 2008; Marek & Janka 2009; B. Müller et al. 2012b).”
Supernova simulations from a 3D progenitor model - Impact of perturbations and evolution of explosion properties (2017, methodology): “Following Wongwathanarat et al. (2010, 2013), we evaluate the proto-neutron star angular momentum JPNS by integrating the flux of angular momentum across the sphere with radius r0, dJPNS dt = ∫ αφ4r20ρvrv × r dΩ.”
Three-dimensional neutrino-driven supernovae: neutron star kicks, spins, and asymmetric ejection of nucleosynthesis products (2012, methodology): “Our analysis, compared to the 2D results of Scheck et al. (2006), reveals that in the 3D case the direct hydrodynamical momentum transfer by gas downflows to and outflows from the NS is much less important than in 2D.”
THE LANDSCAPE OF THE NEUTRINO MECHANISM OF CORE-COLLAPSE SUPERNOVAE: NEUTRON STAR AND BLACK HOLE MASS FUNCTIONS, EXPLOSION ENERGIES, AND NICKEL YIELDS (2014, methodology): “Explosion energy There are a few positive and negative contributions to the supernova explosion energy, which are summarized in Scheck et al. (2006) and Ugliano et al. (2012).”
DELAYED NEUTRINO-DRIVEN SUPERNOVA EXPLOSIONS AIDED BY THE STANDING ACCRETION-SHOCK INSTABILITY (2007, background): “The possibility of such stable accretion with downflows from one (or more) direction(s) and gas outflow in the other direction(s) was indeed seen in the simulations of Scheck et al. (2006).”
Nebular emission-line profiles of Type Ib/c supernovae - Probing the ejecta asphericity (2009, background): “Line shifts such as those observed in [O i] could, in principle, arise from a one-sided ejecta geometry, caused for instance by low-mode convective instabilities (Scheck et al. 2004, 2006; Kifonidis et al. 2006) or the Standing Accretion Shock Instability (SASI; Blondin et al. 2003).”
Protoneutron star evolution and the neutrino-driven wind in general relativistic neutrino radiation hydrodynamics simulations (2009, methodology): “The simulations are then continued applying a simplified radiation hydrodynamics description (see Scheck et al. (2006)), assuming large luminosities to trigger neutrino driven explosions in spherical symmetry.”
Gravitational wave signals from 3D neutrino hydrodynamics simulations of core-collapse supernovae (2016, background): “…of supernovae and their remnants (e.g. mixing in the envelope, see Wongwathanarat, M¨uller & Janka 2015 and references therein; pulsar kicks, Scheck et al. 2006; Wongwathanarat, Janka & M¨uller 2010; Nordhaus…”
NEUTRINO-DRIVEN SUPERNOVA OF A LOW-MASS IRON-CORE PROGENITOR BOOSTED BY THREE-DIMENSIONAL TURBULENT CONVECTION (2015, background): “3), because it is provided mainly by the recombination of free nucleons to α-particles and irongroup nuclei in the gain layer (see Scheck et al. 2006) and the corresponding mass at tpb > 300 ms is only 2.2×10−3 M in 1D.”
Formation of Double Neutron Star Systems (2017, background): “…non-radial hydrodynamic instabilities in the collapsing stellar core (i.e. neutrino-driven convection and the standing accretion-shock instability, Blondin & Mezzacappa 2006; Scheck et al. 2006; Foglizzo et al. 2007; Marek & Janka 2009; Janka 2012, 2013; Bruenn et al. 2014; Foglizzo et al. 2015).”
PROGENITOR-EXPLOSION CONNECTION AND REMNANT BIRTH MASSES FOR NEUTRINO-DRIVEN SUPERNOVAE OF IRON-CORE PROGENITORS (2012, methodology): “The value of the baryonic mass of≤2 M⊙ is safely below the gravitational mass limit of 1.97± 0.04M⊙ set by the recent pre- 4 Note that Scheck et al. (2006) provide an analysis of the energy contributions only for the first second of the explosion.”