Non-spherical core collapse supernovae - II. The late-time evolution of globally anisotropic neutrino-driven explosions and their implications for SN 1987 A

By K. Kifonidis, Tomasz Plewa, L. Scheck, Hans-Thomas Janka, E. M. M. Astrophysics, Garching Center for Astrophys. Thermonucl. Flames, Chicago.. 2005

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Two-dimensional simulations of strongly anisotropic supernova explosions of a nonrotating $15\,M_{\odot}$ blue supergiant progenitor are presented, which follow the hydrodynamic evolution from times shortly after shock formation until hours later. It is shown that explosions which around the time of shock revival are dominated by low-order unstable modes (i.e. by a superposition of the $l=2$ and $l=1$ modes, in which the former is strongest), are consistent with all major observational features of SN 1987 A, in contrast to models which show high-order mode perturbations only and were published in earlier work. Among other items, the low-mode models exhibit final iron-group velocities of up to ${\sim} 3300$ km s -1 , strong mixing at the He/H composition interface, with hydrogen being mixed downward in velocity space to only 500 km s -1 , and a final prolate anisotropy of the inner ejecta with a major to minor axis ratio of about 1.6. The success of low-mode explosions with an energy of about $2\times10^{51}$ erg to reproduce these observed features is based on two effects: the (by 40%) larger initial maximum velocities of metal-rich clumps compared to our high-mode models, and the initial global deformation of the shock. The first effect protects the (fastest) clumps from interacting with the strong reverse shock that forms below the He/H composition interface, by keeping their propagation timescale through the He-core shorter than the reverse shock formation time. This ensures that the outward motion of the clumps remains always subsonic, and that thus their energy dissipation is minimal (in contrast to the supersonic case). The second effect is responsible for the strong inward mixing of hydrogen: the aspherical shock deposits large amounts of vorticity into the He/H interface layer at early times (around $t = 100$ s). This triggers the growth of a strong Richtmyer-Meshkov instability that results in a global anisotropy of the inner ejecta at late times (i.e. around $t = 10\,000$ s), although the shock itself has long become spherical by then. The simulations suggest a coherent picture, which explains the observational data of SN 1987 A within the framework of the neutrino-driven explosion mechanism using a minimal set of assumptions. It is therefore argued that other paradigms, which are based on (more) controversial physics, may not be required to explain this event.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/f4586680dce0e839950e19df58dfea30fd7c6773

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Citations in the corpus

DELAYED NEUTRINO-DRIVEN SUPERNOVA EXPLOSIONS AIDED BY THE STANDING ACCRETION-SHOCK INSTABILITY (2007, background): “…in many supernovae and that seem to determine the appearance of their gaseous remnants might be a consequence of the pronounced asymmetry of the developing blast waves in our simulations (see Kifonidis et al. (2006) for studies of the long-time evolution of anisotropic neutrino-driven explosions).”
SASI ACTIVITY IN THREE-DIMENSIONAL NEUTRINO-HYDRODYNAMICS SIMULATIONS OF SUPERNOVA CORES (2013, background): “Convection and the SASI also create seed asymmetries that determine the ejecta morphology during the explosion phase (Kifonidis et al. 2003, 2006).”
Experimental astrophysics with high power lasers and Z pinches (2004, background): “An interesting new 2D computational study Kifonidis et al., 2006 offers a different approach to breaking the spherical symmetry of the explosion.”
Three-dimensional simulations of core-collapse supernovae: from shock revival to shock breakout (2014, methodology): “Kifonidis et al. (2006) improved the explosion models by replacing the neutrino light-bulb scheme used in Kifonidis et al. (2003) with a ray-by-ray gray neutrino transport approximation (see Scheck et al. 2006, for details).”
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).”
On the nature of supernovae Ib and Ic (2012, methodology): “…originating from our binary-star progenitors, we use a ‘boxcar’ algorithm to modulate the species distribution in the ejecta and hence mimic multidimensional effects associated with massive-star explosions (Kifonidis et al. 2003, 2006; Joggerst, Woosley & Heger 2009; Hammer, Janka & Müller 2010).”
The nebular spectra of SN 2012aw and constraints on stellar nucleosynthesis from oxygen emission lines (2013, background): “…a uniform distribution of 56Ni and O clumps between zero and 1800 km s−1, a scenario that emerges by Rayleigh-Taylor mixing in the explosion (e.g. Kifonidis et al. 2006) and is empirically supported by the observed similarity between iron and oxygen emission line profiles (J12, see also Fig.”
A TWO-PARAMETER CRITERION FOR CLASSIFYING THE EXPLODABILITY OF MASSIVE STARS BY THE NEUTRINO-DRIVEN MECHANISM (2015, unknown): “2), thus improving the simpler, time-dependent boundary neutrino luminosity prescribed by Kifonidis et al. (2006), Scheck et al. (2004, 2006, 2008), and Arcones et al. (2007); Arcones & Janka (2011) and the even simpler neutrino light-bulb treatment (without any transport approximation) applied by…”
NEW TWO-DIMENSIONAL MODELS OF SUPERNOVA EXPLOSIONS BY THE NEUTRINO-HEATING MECHANISM: EVIDENCE FOR DIFFERENT INSTABILITY REGIMES IN COLLAPSING STELLAR CORES (2012, background): “…the morphology of the explosion in the later phases, and are thus a crucial factor for the mixing instabilities in supernovae (Arnett et al. 1989; Kifonidis et al. 2003, 2006; Hammer et al. 2010), the development of pulsar kicks (Janka & Müller 1994; Herant 1995; Burrows & Hayes 1996; Scheck et…”
Multidimensional supernova simulations with approximative neutrino transport. I. Neutron star kicks and the anisotropy of neutrino-driven explosions in two spatial dimensions (2006, background): “Scheck et al. (2004) suggested a link of these low-mode instabilities of the supernova shock during the neutrino-heating phase to global explosion asymmetries (see in particular Kifonidis et al. 2006) and pulsar kicks.”
The 44Ti-powered spectrum of SN 1987A (2011, background): “…comes from theoretical considerations (e.g. Mueller et al. 1991), multi-dimensional simulations (e.g. Herant & Benz 1991; Mueller et al. 1991; Kifonidis et al. 2006; Hammer et al. 2010), the early emergence of X-rays and gamma-rays (Dotani et al. 1987; Pinto & Woosley 1988), and from the…”
Spectropolarimetry of Supernovae (2008, background): “…& Woosley, 1999; Wheeler et al. 2000; Wheeler, Meier & Wilson 2002; Shibata et al. 2003; Maeda & Nomoto 2003; Kotake et al. 2004; Yamada & Sawai 2004; Kifonidis et al. 2006; Obergaulinger et al. 2006; Burrows et al. 2006, 2007; Mezzacappa & Blondin 2007; Moiseenko & BisnovatyiKogan 2007;…”
TOWARD REALISTIC PROGENITORS OF CORE-COLLAPSE SUPERNOVAE (2011, background): “…is fast in comparison to the period associated with O shell dynamics, the shell structure may be caught in a distorted state by the explosion shock, giving a non-spherical remnant even if the explosion shock were perfectly spherical (which it is unlikely to be; Kifonidis et al. 2003, 2006).”