Summary of SN session

Current Status:
Still computationally challenging especially in 3D (but going to 3D is necessary!)
In 2D, multiple progenitor models are taken as an initial condition.
Lots of 2D models are trending toward an explosion, but quantitative differences should be investigated in greater detail. 
--- In 2D models, Ni-mass tends to increase, to first-order, with the ZAMS mass. Compactness will be “a” key parameter to understand the trend.
Many multi-D codes are now under development (spectral leakage, IDSA, GR-M1, SPH… ).
Detailed observations (gamma-ray, clumpiness (Ia), Cas A (NuStar), anisotropic element distributions…..).
Ab-initio EOS available, uncertainty of EOS is now constrained by NS observations and nuclear experiments, weak interactions are improving (such as weak magnetism,
nucleon bremsstrahlung). 
MHD explosions could be a possible and interesting r-process site.

Future direction:
-Presupernova models: More fast rotating progenitor models with high magnetic fields are required, especially, to explain the hypernova branch. R. Hirschi et al. (in prep. next year ?).
  -“The” golden progenitor model for SN code comparison should be selected.
  -In addition to compactness, which parameters are important to characterize the progenitor structures (such as C/O mass, density gradient, composition interfaces) ? 

-SN codes: Detailed comparisons between newly-developed codes are urgent: Starting point is to use the golden progenitor model, the same EOS, the same weak interaction rates, Newtonian hydro. Convergence needs to be checked.         
  -Which features are deterministic and which features are stochastic (like shock radius, dominance of SASI or convection, size of the convective eddies …)
  -Improved weak interaction rates need to be implemented (in a tabular form or as a fitting formula?).  

-Comparison with observations: 
   First, we need to explain nucleosynthetic features of SN1987A, Cas A.
 　Underproduction of Ti44 depends on nuclear rates and explosion dynamics.
 　At the same time, Ni56 should match observations.
   The accurate yields are important for galactic chemical evolution models. 

Summary by Kei and Matthias.