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wiki:summary_of_neutron_star_and_dense_matter_working_group [2012/10/10 09:26]
nucastro created
wiki:summary_of_neutron_star_and_dense_matter_working_group [2013/01/10 17:47] (current)
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 === Theory Needs for Dense Matter and Neutron Stars === === Theory Needs for Dense Matter and Neutron Stars ===
-  * A more complete understanding of X-ray bursts, not only the nuclear +  * A more complete understanding of X-ray bursts, not only the nuclear reaction processes which occur during and between bursts, but also the structure and time evolution of the neutron star atmosphere.
-reaction processes which occur during and between bursts, but also the +
-structure and time evolution of the neutron star atmosphere.+
  
-  * Accurate descriptions of the ground state and lowest-lying +  * Accurate descriptions of the ground state and lowest-lying excitations of hot and neutron-rich nuclei. Also, the ground state and excitations of the neutron star crust for both isolated and accreting neutron stars from the surface to the core-crust transition.
-excitations of hot and neutron-rich nuclei. Also, the ground state and +
-excitations of the neutron star crust for both isolated and accreting +
-neutron stars from the surface to the core-crust transition.+
  
-  * Better interactions/​density functionals/​Hamiltonians,​ and improved +  * Better interactions/​density functionals/​Hamiltonians,​ and improved many-body techniques across the nuclear chart. In particular, improvements in the behavior for neutron matter and neutron-rich nuclei. We need precision masses of medium and heavy neutron-rich nuclei.
-many-body techniques across the nuclear chart. In particular, +
-improvements in the behavior for neutron matter and neutron-rich +
-nuclei. We need precision masses of medium and heavy neutron-rich +
-nuclei.+
  
-  * A clear delineation of the systematic uncertainties associated with +  * A clear delineation of the systematic uncertainties associated with the relationship between nuclear matter and the structure of nuclei. What is the uncertainty due to using the wrong interaction/​density functional/​hamiltonian,​ and what is the uncertainty due to the many-body technique (shell model, HFB, RPA, etc.)? We need to know L and S at the few percent level.
-the relationship between nuclear matter and the structure of nuclei. +
-What is the uncertainty due to using the wrong interaction/​density +
-functional/​hamiltonian,​ and what is the uncertainty due to the +
-many-body technique (shell model, HFB, RPA, etc.)? We need to know L +
-and S at the few percent level.+
  
-  * More detailed knowledge of hypernuclear interactions,​ especially +  * More detailed knowledge of hypernuclear interactions,​ especially three-body interactions involving hyperons such as NN-Lambda and NN-Sigma^{-}. (EOS from the ground up)
-three-body interactions involving hyperons such as NN-Lambda and +
-NN-Sigma^{-}. (EOS from the ground up)+
  
-  * Better calibration of models of intermediate-energy heavy-ion +  * Better calibration of models of intermediate-energy heavy-ion collisions: BUU, QMD, next-generation models? Deeper connection to QMC and CEFT?
-collisions: BUU, QMD, next-generation models? Deeper connection to QMC +
-and CEFT?+
  
-  * Understanding the limits of chiral effective theory: how high can we +  * Understanding the limits of chiral effective theory: how high can we go in density for both neutron and nuclear matter? What is the systematic uncertainty associated with the cutoffs? How far can quantum Monte Carlo go? Why are the three-nucleon interactions from these two approaches so different?
-go in density for both neutron and nuclear matter? What is the +
-systematic uncertainty associated with the cutoffs? How far can quantum +
-Monte Carlo go? Why are the three-nucleon interactions from these two +
-approaches so different?+
  
-  * A clear delination of the nuclear physics input needed for +  * A clear delination of the nuclear physics input needed for core-collapse supernovae simulations:​ EOS, neutrino opacities, electron capture rates, etc. How does the progenitor determine the neutron star mass, spin, and magnetic field? Can we accurately predict the proto-neutron star neutrino signal?
-core-collapse supernovae simulations:​ EOS, neutrino opacities, +
-electron capture rates, etc. How does the progenitor determine the +
-neutron star mass, spin, and magnetic field? Can we accurately predict +
-the proto-neutron star neutrino signal?+
  
wiki/summary_of_neutron_star_and_dense_matter_working_group.txt · Last modified: 2013/01/10 17:47 (external edit)