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Conduct activities to determine the proton number, nucleon number and the number of protons, electrons and neutrons of an atom.
1 015009 (2008) Nij CDBonn Av18 N3LO Nij93 120 60 3 S1 0 0 50 100 150 200 250 E [MeV] •Non-uniqueness of nucleon forces ✘ 2 Complications NN interaction is not unique Strong short-range correlations Carlson et al., Phys.
Strongest spectral lines in the nuclear-physics part of the gamma-ray domain between ' 0.1 and 10 MeV, and their characteristics energy (MeV) 0.078 0.122 0.478 0.511 0.847 1.157 1.173 1.275 1.332 1.634 1.809 2.230 2.313 2.754 4.438 6.129 source process astrophysical origin (source type) ccSN interior nucleosynthesis supernova nucleosynthesis nova nucleosynthesis nucleosynthesis, compact stars, dark matter supernova nucleosynthesis ccSN interior nucleosynthesis ccSN ejected nucleosynthesis nova nucleosynthesis ccSN ejected nucleosynthesis cosmic ray / ISM interactions massive-star and ccSN nucleosynthesis energetic nucleon interactions cosmic ray / ISM interactions cosmic ray / ISM interactions cosmic ray / ISM interactions cosmic ray / ISM interactions radioactive decay:
Erler, et.al 2012 b<0 b=0 b>0 Orsay, 2-6.10.2017 Skyrme EDF • The key ingredient of the nuclear DFT is the nuclear energy density functional (EDF) • The EDF incorporates complex many-body correlations within the energy density constructed from the nucleon densities and currents • Currently there are three major EDF variants in the market:
This mass difference appears in the approximation for the survivability of muon neutrinos 1.4 Super-Kamiokande Experiment The Super-Kamiokande (Super-K) detector was built as a successor to the KamiokaNDE (Kamiokande Nucleon Decay Experiment) detector.