Neutrino-driven Winds in Three-dimensional Core-collapse Supernova Simulations

In this paper, we analyze the neutrino-driven winds that emerge in 12 unprecedentedly long-duration 3D core-collapse supernova simulations done using the code Fornax. The 12 models cover progenitors with zero-age main-sequence mass between 9 and 60 solar masses. In all our models, we see transonic outflows that are at least 2 times as fast as the surrounding ejecta and that originate generically from a proto-neutron star surface atmosphere that is turbulent and rotating. We find that winds are common features of 3D simulations, even if there is anisotropic early infall. We find that the basic dynamical properties of 3D winds behave qualitatively similarly to those inferred in the past using simpler 1D models, but that the shape of the emergent wind can be deformed, very aspherical, and channeled by its environment. The thermal properties of winds for less massive progenitors very approximately recapitulate the 1D stationary solutions, while for more massive progenitors they deviate significantly owing to aspherical accretion. The Y e temporal evolution in winds is stochastic, and there can be some neutron-rich phases. Though no strong r-process is seen in any model, a weak r-process can be produced, and isotopes up to 90Zr are synthesized in some models. Finally, we find that there is at most a few percent of a solar mass in the integrated wind component, while the energy carried by the wind itself can be as much as 10%-20% of the total explosion energy.

Automated summary

In this paper, the researchers conducted 12 unprecedentedly long-duration 3D core-collapse supernova simulations to study the neutrino-driven winds. The results show that the winds in the simulations have transonic outflows that are faster than the surrounding ejecta and originate from a turbulent and rotating proto-neutron star surface atmosphere. The researchers also found that the winds exhibit deformations, aspherical shapes, and can be channeled by their environment. The thermal properties of the winds behave differently for progenitors of different masses, with the less massive progenitors showing similarities to 1D stationary solutions and the more massive progenitors deviating significantly due to aspherical accretion. Additionally, the researchers observed stochastic temporal evolution in the Y e (electron fraction) of the winds and the production of some neutron-rich isotopes. Although no strong r-process was observed, weak r-processes were found to occur, resulting in the synthesis of isotopes up to 90Zr in some models. The integrated wind component was found to be at most a few percent of a solar mass, while the energy carried by the wind itself could be as much as 10%-20% of the total explosion energy.