1. EOS discussion

2. Most important open questions and things to be done
Keeping the astrophysical application in mind (core-collapse supernovae, NS mergers, GRBs, nucleosynthesis, gravitational waves … )
Show slides if you want!

3. Cluster formation, medium modifications, non-uniform matter
Significant modeling required
Uniform nuclear matter: ab-inito approaches, many-body microscopic, and realistic forces vs. phenomenological approaches
Are well calibrated DFTs enough?
How far can we go with ab-initio?
Distinguish high/low T and rho
Saturation point, up to 2 rho and low T under control (?)

4. Missing constraints at high densities besides 2 M_sun
Perspective: Information from short GRBs (e.g. extraction of real M_max), but astrophysical understanding complete?
Use all available information
identify unambiguous constraints, vs. general EOS influence
Gravitational waves, NS mergers
more finite T, Y_e, and different composition EOS needed and simulations for extraction of EOS properties
Realistic EOS, include weak interactions
Conditions for nucleosynthesis, Y_e, dependence on EOS
High magnetic fields
Influence on the crust, e.g. cooling of magnetars via transport and elastic properties
Realistic values, and for which timescales persistent
General question of equilibrium and timescales and EOS

5. Eos at high temperatures, T>TF
Additional baryonic/mesonic DoFs: Hyperons, Deltas, Pions
Hyperon puzzle solved?
Quark matter
At which density/temperature?
Absolute stability?
Reliable models?
Problem of MIT bag (also NJL): unknown parameters
Better approaches available or not?
Maximum mass problem in other approaches
Isospin dependence
Chiral invariant and confining
Similar problems in heavy-ion collisions
Missing baryonic DoFs
«Nature» of quark-hadron phase coexistence
Kind/order of QCD phase transition

6. Phase transitions
Correct treatment? Which one?
EOS tables for astrophysical simulations
Current status satisfactory?
best-fit vs. variety of models
Compose database
Format of tables (T, n_B, Y_e good?)
Solid conversion to other formats (energy or entropy)
Polynomial fits
Neutrino response and transport properties
Unified description, also for clusterized/non-uniform matter?
Off-equilibrium crucial for neutrino opacities

7. Ideas for new astrophysical phenomenology/scenarios
Burning to quark matter, Quarknova, transition to third family in mergers, …
Strategy?