Energy levels of light nuclei A=8,9,10

Energy levels of A = 21−44 nuclei (V)

https://www.cns.s.u-tokyo.ac.jp/~shimoura/research/nuc_data/pdf/19.pdf

Energy levels of light nuclei A=11☆

Total cross sections for the production of gamma-ray lines from nuclear deexcitation as a function of the projectile energy are evaluated and presented. Included are proton and α reactions with He, C, N, O, Ne, Mg, Al, Si, S, Ca, and Fe. Such functions are essential for interpretation of gamma-ray line observations of astrophysical sites which contain large fluxes of energetic particles such as solar flares, the Earth's atmosphere, planetary atmospheres and surfaces, the interstellar medium, and galactic nebulae.

https://iopscience.iop.org/article/10.1086/340545/pdf

Nuclear Deexcitation Gamma-Ray Lines from Accelerated Particle Interactions

Calculations are made of the rates at which bursts of electronic charge are created in silicon by cosmic rays at sea level. These rates are reduced to two types: point charge bursts and distributed ionization wake bursts. A procedure is shown to evaluate the soft fail rates of simple devices caused by cosmic rays. It is shown that an 8‐M byte semiconductor memory made of 10×10 μm diodes will have a soft fail rate of about one per day.

The effect of sea level cosmic rays on electronic devices

The energy spectra of light nuclides (
 1
 1
 H,
 1
 2
 H,
 1
 3
 H,
 2
 3
 He,
 2
 4
 He) produced in the interaction of 600 MeV protons on various targets (Be, C, Na, Al, Ca, Fe, Au) have been measured at several laboratory angles (30°, 45°, 75°, 105°), by means of ΔE-E telescopes (semiconductor and scintillator detectors). The spectra are fitted with calculated curves derived both from a two-step model and a thermodynamical model of the p-nucleus interaction. Two ranges of nuclear temperature are found: the first one (about (20÷30) MeV) describes the high-energy part of the spectra, the second one (a few MeV) describes the low-energy part (de-excitation of the residual nucleus). These fits are used for the integration over energies and angles, which allows the computation of the total cross-sections and of the fragmentation probabilities. These probabilities are necessary for the study of2H and3He production in the propagation of galactic cosmic rays and their interaction with interstellar matter. We find that the 〈CNO〉 contribution for the production of cosmic He nuclei is not negligible and must be added to the4He contribution. The mean interstellar path length is about 4 g·cm−2. The results obtained with Na and Ca targets should present a biophysical interest.

Light-fragment production in p--nucleus interactions at 600 MeV: astrophysical application

A p-gamma coincidence experiment has been performed with 400-MeV protons The angular and momentum analysis of the scattered proton demonstrates a primary quasifree process The residual nuclei which have been identified from the gamma-ray spectra characterize the final states and indicate an evaporation process or a sequential ejection at low energy of some correlated nucleons In addition, preliminary results with triple coincidences (2p-gamma) indicate a promising way to clarify the mechanism of quasifree reactions

Multinucleon removal in a quasifree process with a p-. gamma. coincidence experiment at 400 MeV

Inclusive cross-sections for the production of3He and4He isotopes in α+α collisions at 218 MeV have been measured, using a semiconductor telescope. We discuss the significance of these measurements for theories of galactic cosmic-ray propagation.

J.P. Alard

Papers

Light-fragment production in p--nucleus interactions at 600 MeV: astrophysical application

Multinucleon removal in a quasifree process with a p-. gamma. coincidence experiment at 400 MeV

Light-fragment production in alpha-alpha collisions at 218 MeV

Nuclear γ-ray production in p-nucleus interactions at high energy

Experimental study of the light isotope production in alpha+alpha interactions