Neutrino-Driven Winds in Three-Dimensional Core-Collapse Supernova Simulations. (arXiv:2306.13712v1 [astro-ph.SR])
<a href="http://arxiv.org/find/astro-ph/1/au:+Wang_T/0/1/0/all/0/1">Tianshu Wang</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Burrows_A/0/1/0/all/0/1">Adam Burrows</a>
In this paper, we analyze the neutrino-driven winds that emerge in twelve
unprecedentedly long-duration 3D core-collapse supernova simulations done using
the code Fornax. The twelve models cover progenitors with ZAMS mass between 9
and 60 solar masses. In all our models, we see transonic outflows that are at
least two times as fast as the surrounding ejecta and that originate
generically from a PNS surface atmosphere that is turbulent and rotating. We
find that winds are common features of 3D simulations, even if there is
anisotropic early fallback. 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 due to aspherical fallback. 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 $^{90}$Zr 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.
In this paper, we analyze the neutrino-driven winds that emerge in twelve
unprecedentedly long-duration 3D core-collapse supernova simulations done using
the code Fornax. The twelve models cover progenitors with ZAMS mass between 9
and 60 solar masses. In all our models, we see transonic outflows that are at
least two times as fast as the surrounding ejecta and that originate
generically from a PNS surface atmosphere that is turbulent and rotating. We
find that winds are common features of 3D simulations, even if there is
anisotropic early fallback. 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 due to aspherical fallback. 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 $^{90}$Zr 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.
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