Non-spherical core collapse supernovae. I. Neutrino-driven convection, Rayleigh-Taylor instabilities, and the formation and propagation of metal clumps

By K. Kifonidis, Tomasz Plewa, Hans-Thomas Janka, E. Mueller. 2003

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We have performed two-dimensional simulations of core collapse supernovae that encompass shock revival by neutrino heating, neutrino-driven convection, explosive nucleosynthesis, the growth of Rayleigh-Taylor instabilities, and the propagation of newly formed metal clumps through the exploding star. A simulation of a type II explosion in a 15 M blue supergiant progenitor is presented, that confirms our earlier type II models and extends their validity to times as late as 5.5 hours after core bounce. We also study a type Ib-like explosion, by simply removing the hydrogen envelope of the progenitor model. This allows for a first comparison of type II and type Ib evolution. We present evidence that the hydrodynamics of core collapse supernovae beyond shock revival diers markedly from the results of simulations that have followed the Rayleigh-Taylor mixing starting from ad hoc energy deposition schemes to initiate the explosion. We find iron group elements to be synthesized in an anisotropic, dense, low-entropy shell that expands with velocities of17 000 km s 1 shortly after shock revival. The growth of Rayleigh-Taylor instabilities at the Si/ Oa nd (C+O)/He composition interfaces of the progenitor, seeded by the flow-structures resulting from neutrino-driven convection, leads to a fragmentation of this shell into metal-rich "clumps". This fragmentation starts already 20 s after core bounce and is complete within the first few minutes of the explosion. During this time the clumps are slowed down by drag, and by the positive pressure gradient in the unstable layers. However, at t 300 s they decouple from the flow and start to propagate ballistically and subsonically through the He core, with the maximum velocities of metals remaining constant at3500 5500 km s 1 . This early "clump decoupling" leads to significantly higher 56 Ni velocities at t= 300 s than in one-dimensional models of the explosion, demonstrating that multi-dimensional eects which are at work within the first minutes, and which have been neglected in previous studies (especially in those which dealt with the mixing in type II supernovae), are crucial. Despite comparably high initial maximum nickel velocities in both our type II and our type Ib-like model, we find that there are large dierences in the final maximum nickel velocities between both cases. In the "type Ib" model the maximum velocities of metals remain frozen in at3500 5500 km s 1 for t 300 s, while in the type II model they drop significantly for t > 1500 s. In the latter case, the massive hydrogen envelope of the progenitor forces the supernova shock to slow down strongly, leaving behind a reverse shock and a dense helium shell (or "wall") below the He/H interface. After penetrating into this dense material the metal-rich clumps possess supersonic speeds, before they are slowed down by drag forces to1200 km s 1 at a time of 20 000 s post-bounce. While, due to this deceleration, the maximum velocities of iron-group elements in SN 1987 A cannot be reproduced in case of the considered 15 M progenitor, the "type Ib" model is in fairly good agreement with observed clump velocities and the amount of mixing inferred for type Ib supernovae. Thus it appears promising for calculations of synthetic spectra and light curves. Furthermore, our simulations indicate that for type Ib explosions the pattern of clump formation in the ejecta is correlated with the structure of the convective pattern prevailing during the shock-revival phase. This might be used to deduce observational constraints for the dynamics during this early phase of the evolution, and the role of neutrino heating in initiating the explosion.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/155e8976cd02ae45c690baa14ff8412a80bd50c4

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Citations in the corpus

PROGENITOR-EXPLOSION CONNECTION AND REMNANT BIRTH MASSES FOR NEUTRINO-DRIVEN SUPERNOVAE OF IRON-CORE PROGENITORS (2012, methodology): “During the long-time simulations of the SN dynamics we follow approximately the explosive nucleosynthesis by solving a small alpha-reactions network, similar to the network described in Kifonidis et al. (2003).”
A NEW MULTI-DIMENSIONAL GENERAL RELATIVISTIC NEUTRINO HYDRODYNAMIC CODE FOR CORE-COLLAPSE SUPERNOVAE. I. METHOD AND CODE TESTS IN SPHERICAL SYMMETRY (2010, background): “…(1994), combining the high resolution of the HLLC solver (Toro et al. 1994; Mignone & Bodo 2005) with the robustness of the HLLE solver (Harten et al. 1983; Einfeldt 1988) against odd–even decoupling near grid-aligned shocks (Quirk 1994; Liou 2000; Kifonidis et al. 2003; Sutherland et al. 2003).”
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).”
CORE-COLLAPSE SUPERNOVAE FROM 9 TO 120 SOLAR MASSES BASED ON NEUTRINO-POWERED EXPLOSIONS (2015, methodology): “The pre-SN models were exploded using two different onedimensional hydrodynamics codes, Prometheus-Hot Bubble (henceforth P-HOTB; Janka & Müller 1996; Kifonidis et al. 2003) and KEPLER.”
Nucleosynthesis-relevant conditions in neutrino-driven supernova outflows. I. Spherically symmetric (2006, methodology): “A detailed description of the numerical method, initial models, and boundary treatment can be found in Paper I, Scheck et al. (2006), and Kifonidis et al. (2003).”
Composition of the Innermost Core-Collapse Supernova Ejecta (2004, background): “It is likely that the discrepancies in Ye are heavily mixed on a dynamical time scale (Kifonidis et al. 2003).”
A TWO-PARAMETER CRITERION FOR CLASSIFYING THE EXPLODABILITY OF MASSIVE STARS BY THE NEUTRINO-DRIVEN MECHANISM (2015, methodology): “…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 Janka & Müller (1996) and Kifonidis et al. (2003).”
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…”
Experimental astrophysics with high power lasers and Z pinches (2004, result): “These 2D simulation results are much more consistent with the observations of SN1987A that previous results from this group Kifonidis et al., 2000, 2003 .”
Three-dimensional neutrino-driven supernovae: neutron star kicks, spins, and asymmetric ejection of nucleosynthesis products (2012, methodology): “In order to follow approximately the explosive nucleosynthesis, we solve a small α-chain reaction network, similar to the network described in Kifonidis et al. (2003).”
Young Core-Collapse Supernova Remnants and Their Supernovae (2004, background): “10 of Matzner & McKee 1999), but this part of the supernova is likely to be affected by Rayleigh-Taylor instabilities in any case (Kifonidis et al. 2003 and references therein).”
Multidimensional supernova simulations with approximative neutrino transport. II. Convection and the (2007, methodology): “We employed the version of the hydrodynamics code that was described by Kifonidis et al. (2003).”
Multidimensional supernova simulations with approximative neutrino transport. I. Neutron star kicks and the anisotropy of neutrino-driven explosions in two spatial dimensions (2006, methodology): “Yet, we point out here that all the previously not modelled neutrino transport effects are not the reason why the development of l = 1, 2 modes is seen here, whereas it was not visible in the calculations of Janka & Müller (1996) and Kifonidis et al. (2003).”
Production of dust by massive stars at high redshift (2011, background): “…be explained by the theoretically observed instability of the nickel bubble during explosion of the SN leading to Rayleigh–Taylor instabilities forming in the post-shocked ejecta (e.g., Chevalier and Klein, 1978; Arnett, 1988; Herant and Benz, 1991; Herant and Woosley, 1994; Kifonidis et al, 2003).”
Two-dimensional hydrodynamic core-collapse supernova simulations with spectral neutrino transport - I. Numerical method and results for a 15 solar mass star (2005, methodology): “…published by EDP Sciences and available at http://www.edpsciences.org/aa or http://dx.doi.org/10.1051/0004-6361:20053783 Supernova 1987A and other supernovae, and which possibly is the origin of many morphological features of supernova remnants (e.g., Kifonidis et al. 2003, and references therein).”