Systematic Features of Axisymmetric Neutrino-Driven Core-Collapse Supernova Models in Multiple Progenitors

Abstract

We present an overview of two-dimensional (2D) core-collapse supernova simulations employing neutrino transport scheme by the isotropic diffusion source approximation. We study 101 solar-metallicity, 247 ultra metal-poor, and 30 zero-metal progenitors covering zero-age main sequence mass from 10.8 M ⊙ to 75.0 M ⊙ . Using the 378 progenitors in total, we systematically investigate how the differences in the structures of these multiple progenitors impact the hydrodynamics evolution. By following a long-term evolution over 1.0 s after bounce, most of the computed models exhibit neutrino-driven revival of the stalled bounce shock at ∼ 200 -800 ms postbounce, leading to the possibility of explosion. Pushing the boundaries of expectations in previous one-dimensional (1D) studies, our results confirm that the compactness parameter ξ that characterizes the structure of the progenitors is also a key in 2D to diagnose the properties of neutrinodriven explosions. Models with high ξ undergo high ram pressure from the accreting matter onto the stalled shock, which affects the subsequent evolution of the shock expansion and the mass of the protoneutron star under the influence of neutrino-driven convection and the standing accretion-shock instability. We show that the accretion luminosity becomes higher for models with high ξ, which makes the growth rate of the diagnostic explosion energy higher and the synthesized nickel mass bigger. We find that these explosion characteristics tend to show a monotonic increase as a function of the compactness parameter ξ.

On the Intrinsic Diversity of Type Ii-Plateau Supernovae

“…In a simple spherical picture, the evolution of the neutrino-driven wind is determined by the thermodynamic structure of the layers below the ejecta mass cut (Pejcha & Thompson 2015), while the ejected mass of 56 Ni depends primarily on the mass of the shock-heated ejecta exposed to sufficiently high temperatures (Weaver & Woosley 1980;Woosley 1988;Thielemann et al 1990). The intrinsic scatter in the E exp -M Ni relation therefore implies that the progenitor structure below and above the mass cut cannot be fully described by a single parameter, such as the compactness (O'Connor & Ott 2011Nakamura et al 2014;Pejcha & Thompson 2015;Perego et al 2015). Using the results of Pejcha & Thompson (2015), we find a width of 0.10 +0.01 −0.01 dex in their E exp -M Ni correlation, which is consistent with the results presented here.…”

“…Heger et al 2003;Nomoto et al 2006;Utrobin & Chugai 2009, there is little evidence from the parameterized studies of the neutrino mechanism that the supernova properties such as E exp or M Ni will strongly correlate with the mass of the progenitor (e.g. O'Connor & Ott 2011; Ugliano et al 2012;Bruenn et al 2014;Nakamura et al 2014;Pejcha & Thompson 2015;Perego et al 2015;Ertl et al 2015), because the ultimate fate of the star and the initiation of the explosion is set by the physics and the thermodynamic structure on the inner ∼ 2.5 M ⊙ of the progenitor, which is not monotonic with the initial mass, metallicity or final hydrogen mass (Sukhbold & Woosley 2014).…”

Pushing Core-Collapse Supernovae to Explosions in Spherical Symmetry. I. The Model and the Case of Sn 1987a

“…A clear correlation between explosion properties and progenitor compactness has been recently discussed by Nakamura et al (2014). They performed systematic 2D calculations of exploding CCSNe for a large variety of progenitors, using the IDSA to model ν e and νe transport.…”

Failure of a Neutrino-Driven Explosion After Core-Collapse May Lead to a Thermonuclear Supernova

“…One-dimensional (1D) simulations indicate that the neutrinos do not deposit sufficient energy in the envelope to produce the typical ∼10 51 erg kinetic energy. While some two-dimensional (2D) studies indicate robust explosions (Bruenn et al 2013(Bruenn et al , 2014Nakamura et al 2014;Suwa et al 2014) and some indicate failures or weak explosions (Takiwaki et al 2014;Dolence et al 2015), these studies are affected by the assumption of rotational symmetry and by an inverse turbulent energy cascade, which, unlike many physical systems, tends to amplify energy on large scales. Therefore, three-dimensional (3D) studies are necessary to satisfactorily demonstrate the neutrino mechanism, but so far 3D studies have resulted in either failures or weak explosions (Takiwaki et al 2014;Lentz et al 2015;Melson et al 2015a,b).…”