A Consistent Modeling of Neutrino-driven Wind with Accretion Flow onto a Protoneutron Star and its Implications for ${}^{56}$Ni Production

Abstract

Details of the explosion mechanism of core-collapse supernovae (CCSNe) are not yet fully understood. There is now an increasing number of successful examples of reproducing explosions in the first-principles simulations, which have shown a slow increase of explosion energy. However, it was recently pointed out that the growth rates of the explosion energy of these simulations are insufficient to produce enough ${}^{56}$Ni mass to account for observations. We refer to this issue as the `nickel mass problem' (Ni problem, hereafter) in this paper. The neutrino-driven wind is suggested as one of the most promising candidates for the solution to the Ni problem in previous literature, but a multi-dimensional simulation for this is computationally too expensive to allow long-term investigations. In this paper, we first built a consistent model of the neutrino-driven wind with an accretion flow onto a protoneutron star (PNS), by connecting a steady-state solution of the neutrino-driven wind and a phenomenological mass accretion model. Comparing the results of our model with the results of first-principles simulations, we find that the total ejectable amount of the neutrino-driven wind is roughly determined within $\sim$ 1 sec from the onset of the explosion and the supplementable amount at a late phase ($t_e\gtrsim 1$ sec) remains $M_{\mathrm{ej}}\lesssim 0.01M_{\odot }$ at most. Our conclusion is that it is difficult to solve the Ni problem, by continuous injection of ${}^{56}$Ni by the neutrino-driven wind. We suggest that the total amount of synthesized ${}^{56}$Ni can be estimated robustly if simulations are followed up to $\sim 2$ seconds.

arXiv comment11 pages, 6 figures, 1 table, accepted for publication in ApJ

References in corpus (31)

• Explosion Mechanisms of Core-Collapse Supernovae
• Core-Collapse Supernovae from 9 to 120 Solar Masses Based on Neutrino-powered Explosions
• Nucleosynthesis in neutrino-driven winds: I. The physical conditions
• Progenitor-Explosion Connection and Remnant Birth Masses for Neutrino-Driven Supernovae of Iron-Core Progenitors
• Observed and Physical Properties of Core-Collapse Supernovae
• Protoneutron star evolution and the neutrino driven wind in general relativistic neutrino radiation hydrodynamics simulations
• Core-Collapse Supernova Explosion Theory
• Neutrino Signal of Electron-Capture Supernovae from Core Collapse to Cooling
• A two-parameter criterion for classifying the explodability of massive stars by the neutrino-driven mechanism
• The r-process nucleosynthesis in the various jet-like explosions of magnetorotational core-collapse supernovae
• The Physics of Protoneutron Star Winds: Implications for r-Process Nucleosynthesis
• The Overarching Framework of Core-Collapse Supernova Explosions as Revealed by 3D Fornax Simulations
• High Resolution Study of Presupernova Compactness
• A Simple Approach to the Supernova Progenitor-Explosion Connection
• General relativistic effects on neutrino-driven wind from young, hot neutron star and the r-process nucleosynthesis
• The neutrino signal from protoneutron star accretion and black hole formation
• The r-Process in Neutrino-Driven Winds from Nascent, "Compact" Neutron Stars of Core-Collapse Supernovae
• The Development of Explosions in Axisymmetric Ab Initio Core-Collapse Supernova Simulations of 12-25 $M_{\odot }$ Stars
• The r-process in proto-neutron-star wind revisited
• Nucleosynthesis in the Innermost Ejecta of Neutrino-Drive Supernova Explosions in Two Dimensions
• Production and Distribution of ${}^{44}$Ti and ${}^{56}$Ni in a Three-dimensional Supernova Model Resembling Cassiopeia A
• Investigating the properties of stripped-envelope supernovae, what are the implications for their progenitors?
• A New Multi-Dimensional General Relativistic Neutrino Hydrodynamics Code for Core-Collapse Supernovae IV. The Neutrino Signal
• Hydrodynamical study of neutrino-driven wind as an r-process site
• Nucleosynthesis in 2D Core-Collapse Supernovae of 11.2 and 17.0 M${}_{\odot }$ Progenitors: Implications for Mo and Ru Production
• The criterion of supernova explosion revisited: the mass accretion history
• Importance of ${}^{56}$Ni production on diagnosing explosion mechanism of core-collapse supernova
• Survey of astrophysical conditions in neutrino-driven supernova ejecta nucleosynthesis
• Nucleosynthesis Constraints on the Energy Growth Timescale of a Core-collapse Supernova Explosion
• Nucleosynthesis in neutrino-driven winds in hypernovae
• Proton-Rich Nuclear Statistical Equilibrium

Cited by in corpus (8)

• Self-consistent 3D Supernova Models From -7 Minutes to +7 Seconds: a 1-bethe Explosion of a ~19 Solar-mass Progenitor
• Three-dimensional simulation of a core-collapse supernova for a binary star progenitor of SN 1987A
• On the energy source of ultra-stripped supernovae
• Are stripped envelope supernovae really deficient in ${}^{56}$Ni?
• Deep Learning of the Eddington Tensor in the Core-collapse Supernova Simulation
• X-raying the Birth of Binary Neutron Stars and Neutron Star-Black Hole Binaries
• Gravitational Collapse of White Dwarfs to Neutron Stars. I. From Initial Conditions to Explosions with Neutrino-radiation Hydrodynamics Simulations
• Constraints on Explosion Timescale of Core-Collapse Supernovae Based on Systematic Analysis of Light Curves