Abstract
Abstract We present a new method for neutrino-matter coupling in multi-dimensional radiation-hydrodynamic simulations of core-collapse supernovae (CCSNe) with the full Boltzmann neutrino transport. This development is motivated by the fact that accurate conservation of momentum is required for reliable numerical modelings of CCSN dynamics including a recoil of proto-neutron stars (PNSs). The new method is built on a hybrid approach in which we use the energy-momentum tensor of neutrinos to compute the momentum feedback from neutrino to matter in the optically thick region while we employ the collision term in the optically thin region. In this method we utilize a general relativistic description of radiation-hydrodynamics with angular moments, which allows us to evaluate the momentum feedback from neutrino to matter without inconsistency with our Boltzmann solver. We demonstrate that the new method substantially improves the accuracy of linear momentum conservation in our CCSN simulations under reasonable angular resolutions in momentum space, alleviating the difficulty in giving the diffusion limit precisely with the discrete ordinate (S n ) method. It is the first ever demonstration that the PNS kick can be handled directly and properly in multi-dimensional radiation-hydrodynamic simulations with the full Boltzmann neutrino transport.
Highlights
For practical reasons, it is truncated at a certain level: First-principles numerical modeling of core-collapse most of the schemes normally treat moments up to the supernova (CCSN) is an indispensable approach to re-0th or 1st order
We present a new method for neutrino-matter coupling in multi-dimensional radiation-hydrodynamic simulations of core-collapse supernova (CCSN) with the full Boltzmann neutrino transport
We develop a new method for the neutrino-matter coupling to improve the accuracy of the linear momentum conservation in multi-D CCSN simulations with the angular-grid-based Boltzmann solver for neutrino transport
Summary
It is truncated at a certain level: First-principles numerical modeling of core-collapse most of the schemes normally treat moments up to the supernova (CCSN) is an indispensable approach to re-. Energy and momentum in neutrino transport (see e.g., One of the numerical challenges in addressing the issue is Shibata et al (2011)). The conservative form of GR Boltztion in Boltzmann-radiation-hydrodynamics simulations mann equation implemented in our code satisfies only of CCSNe. We first give a brief overview of our CCSN code and the energy and momentum is violated in general once some relevant differences from others. Other state-of-the-art numerimethod alleviates the shortcoming of the Boltzmann cal simulations have employed some approximations solver and allows us to overcome the problem with comfor neutrino transport
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