Multi-D Code Comparison - first steps

Goals

The goal is to create a simple yet complete set of conditions that can be easily simulated by many core-collapse groups. We want to strictly adhere to the same procedure for everything to minimize differences. Below we outline in detail the conditions for our tests, please comment if these are too strict, not strict enough, or if other conditions need to be considered.

Discussion on Initial Conditions

Oak Ridge cannot, as of yet, perform simulations with non-LS EOS. This presents a problem as this below set of initial conditions prevents their participation. The alternative, which is using the one of the LS EOS, is also undesirable because it opens up the can of worms that is low density EOS treatments, this was the reason for proposing the use the SFHo EOS, because it provides pressures (however inconsistent with reality) down to very low densities (1 g/ccm).

Anyone have any suggestions? Does anyone want to do a LS220 simulation in addition to the SFHo simulation to provide a connect?

Initial Conditions

Non-neutrino Physics

  1. Progenitor: \(20\,M_\odot\) model from (WOOSLEY 2007). This model is available from the authors. Ideally, we would compare both a successful explosion and a failed explosion to test codes in both regimes. For this, we may need to add a second progenitor at a later stage. After seeing the outcome of these simulations.

  2. For mapping the progenitor, we will use density, temperature, and ye. Careful to note the definition of the radial coordinate in the initial model (radial coordinate is the location of the outer edge of the zone, the velocity is also defined at this radius, the remaining required quantities (rho, temperature, ye) are defined as cell averages).

  3. Equation of state: The SFHo nuclear equation of state from (Steiner 2013) available from http://phys-merger.physik.unibas.ch/~hempel/eos.html or http://www.stellarcollapse.org/equationofstate. This EOS extends down to densities of \(1\,\mathrm{g}\,\mathrm{cm}^{-3}\). In this EOS, NSE is assumed down to these densities (which is incorrect for supernovae). However, to eliminate (for now) issues related to low density equations of state and nuclear reaction networks, this study will use only the SFHo equation of state for all densities, temperatures, and ye’s.

  4. Boundary and Boundary Conditions: The SFHo EOS only goes