Neutron Stars Chandrasekhar limit on white dwarf mass Supernova explosions –Formation of elements (R, S process) –Neutron stars –Pulsars Formation of X-Ray.
Introduction General principles Today: quantitative theory; predictive capability Challenges for tomorrow Summary Nuclear Structure Theory: today and tomorrow.
(Some of the possible) Astrophysical origins of high energy cosmic rays Diego F. Torres [email protected] Lawrence Livermore Lab. California, 94550,
+ 2 208 Pb Electroweak Asymmetry in Elastic Electron-Nucleus Scattering -- Weak charge form factor -- most weak charge is carried by neutrons PREX and.
Excitation of Supernova Remnants by Twisting of the Neutron Star Dipole Magnetic Flux
2 Excitation of Supernova Remnants by Twisting of the Neutron Star Dipole Magnetic Flux Stirling Colgate, LANL with Hui Li, LANL & Ken Fowler, UC Berkley,
