Connecting nuclei to nucleon matter:
Year 1: Pairing gap and neutron matter EoS up to supra nuclear density.
Year 2: Benchmarks for nuclear matter EoS at zero temperature using QMC
Year 3: EoS table for supernova simulations using QMC at T=0 to provide benchmarks.
Year 4: QMC results for finite temperature neutron matter.
Year 5: EoS for supernova with finite temperature QMC benchmarks.
Weak interactions in nuclei and neutrino reactions:
Year 1: Low energy neutrino-nucleus cross-sections in HFB.
Year 2: Spin and density response functions for weak interaction in neutron matter.
Year 3: Results for neutrino-nucleus and neutrino cross-sections in nuclear matter of relevance to supernova with improved energy functionals.
Year 4: Code to calculate nuclear weak interaction rates at finite temperature for astrophysical applications.
Year 5: Cross sections for neutrino detectors and supernova neutrino transport.
Neutrino flavor transformations:
Year 1: Results for 3x3 multi-angle neutrino flavor transformations
Year 2: Results for 3x3 multi-angle neutrino flavor transformations, exploration of diverse supernovae environments.
Year 3: Results for collective neutrino transformations with multidimensional effects and small scale turbulence.
Year 4: Towards a unified treatment of coherent and incoherent neutrino interactions.
Year 5: Impact, observability and constraints on supernova conditions and neutrino properties from flavor transformations in supernova.
Year 1: Impact of single angle collective neutrino transformations on ambient conditions and composition: (i) Results for r-process abundances with single angle collective neutrino transformations; (ii) Helium zone neutrino induced r-process.
Year 2: Revised beta decay reaction rates in r-process networks and sensitivity analysis.
Year 3: Results for progenitor structure for nucleosynthesis in O-Ne-Mg supernova.
Year 4: Predict elemental abundances in SN and accretion disks using revised rates and neutrino fluxes.
Year 5: Nucleosynthesis calculations using latest suite of supernova simulations and neutrino luminosities.
Neutron Stars and Phase Transitions:
Year 1: Thermal conductivity and structure of the inner NS crust. Composition of accreting neutron star crust.
Year 2: Composition and conductivity of accreting NS crusts. Model independent NS EOS from simultaneous mass-radius measurements . Determine under what circumstances the CFL-K0 phase can be treated as a two-component superfluid and explore its consequences for neutron star modes.
Year 3: Hydrodynamic description and viscosity of superfluid quark matter and NS oscillations.
Year 4: Spectrum of shear modes in magnetized NS crusts. Vortex structure in multi-component fluids and vortex-vortex interactions in the nuclear superfluid. Establish conditions under which exotic vortex states can arise.
Year 5: Mass-radius predictions for nucleonic and hybrid NS neutron stars with quark cores with updated EoS. Phenomenology of the surface of a CFL quark star, search for distinctive features in comparison with surfaces of different composition.
Year 1: Predict neutrino emission from protoneutron stars in 1-d using modern initial conditions and existing microphysics.
Year 2: X-ray burst (XRB) simulations, NS structure and library of ash compositions in 1-d.
Year 3: Thermal profiles and superbursts in accreting neutron star and light-curves.
Year 4: Results with Monte Carlo neutrino transport code with updated microphysics.
Year 5: Suite of predictions for supernova neutrino signal including the microphysics and neutrino flavor transformation. Burst light-curves and transients and relation to NS properties.