The measured flux averaged cross sections on oxygen nuclei are langle σ ν rm ncqe. Neutrino and antineutrino oxygen neutral current quasielastic like interactions are measured at super kamiokande using nuclear de excitation γ rays to identify signal like interactions in data from a 14 94 16 35 times 10 20 protons on target exposure of the t2k neutrino antineutrino beam. If an atomic nucleus absorbs an electron of the right energy it can.
Experimental evidence is presented for isomer depletion through nuclear excitation by electron capture in molybdenum 93 nuclei. Its photon energy distribution. 1 2009 nuclear gamma ray de excitation lines and continuum 143 the unresolved line continuum has not been addressed since thefirstapproximationbyrkl intherklgamma raylinepro duction code this component was treated as a true continuum peaking in the 1 2 mev region.
In this paper we use. The energies and widths of γ ray lines provide a wealth of information on the directionality and spectra of ions in solar flares. Since almost all de excitation lines from nuclear states excited by flare accelerated protons and α particles are emitted promptly after nuclear collisions the emission photon s energy depends on the velocity of the recoiling nucleus.
Photons are bundles of radiant energy that represent the particle nature of light. Excitation occurs when a ground state electron absorbs a photon and jumps up to a higher unstable energy level. Those electrons which are free to vibrate without striking neighboring atoms complete two quantum mechanical processes.
The brightness and evolution of these lines constrains the spectrum and composition of the accelerated particles and the composition of the local atmosphere. During large flares nuclei in the solar atmosphere which have experienced interactions with accelerated protons and other ions emit de excitation gamma rays characteristic of each element. Although it has always been included in the code its photon energy distribution had been estimated from.
This continuum consists of all emission not accounted for by the explicit lines included in the line production code. Second for the first time we give a full and detailed evaluation of the nuclear de excitation unresolved line continuum. For the nucleus of lead 206 as an example the excitation energy of the first excited state is 0 80 million electron volts and of the second excited state 1 18 million electron volts.
Nuclear excitation energies are roughly 1 000 000 times greater than atomic excitation energies.
Nuclear de excitation. The most stable nuclear isomer occurring in nature is 180m 73 ta which is present in all tantalum samples at about 1 part in 8 300. Its half life is at least 10 15 years markedly longer than the age of the universe. The low excitation energy of the isomeric state causes both gamma de excitation to the 180 ta. A nuclear line de excitation spectrum including those c and o lines may be expected also from particle acceleration sites and sources as energetic particles interact with ambient gas within or.
A nuclear line de excitation spectrum including those c and o lines may be expected also from particle acceleration sites and sources as energetic particles interact with ambient gas within or. The low excitation energy of the isomeric state causes both gamma de excitation to the 180 ta. Its half life is at least 10 15 years markedly longer than the age of the universe.
The most stable nuclear isomer occurring in nature is 180m 73 ta which is present in all tantalum samples at about 1 part in 8 300.
