Cosmic-ray study of properties of nuclear interactions in the 10-300-GeV energy range
Cosmic ray nuclear interactions in 10-300 GeV energy range, using balloon-borne emulsion target, spark chambers and ionization spectrometer
Goza, E. R.↗
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High energy hadrons in extensive air showers
Experimental data on the high energy hadronic component in extensive air showers of energies approx. 10 to the 14 to 10 to the 16 eV when compared with expectations from Monte Carlo simulations have shown the observed showers to be deficient in high energy hadrons relative to simulated showers. An attempt is made to understand these anomalous features with more accurate comparison of observations with expectations, taking into account the details of the experimental system. Results obtained from this analysis and their implications for the high energy physics of particle interactions at energy approx. 10 to the 15 eV are presented.
Tonwar, S. C.↗
Description of alpha-nucleus interaction cross sections for cosmic ray shielding studies
Nuclear interactions of high-energy alpha particles with target nuclei important for cosmic ray studies are discussed. Models for elastic, quasi-elastic, and breakup reactions are presented and compared with experimental data. Energy-dependent interaction cross sections and secondary spectra are presented based on theoretical models and the limited experimental data base.
Cucinotta, Francis A.↗
Energy Transfer and Triadic Interactions in Compressible Turbulence
Using a two-point closure theory, the Eddy-Damped-Quasi-Normal-Markovian (EDQNM) approximation, we have investigated the energy transfer process and triadic interactions of compressible turbulence. In order to analyze the compressible mode directly, the Helmholtz decomposition is used. The following issues were addressed: (1) What is the mechanism of energy exchange between the solenoidal and compressible modes, and (2) Is there an energy cascade in the compressible energy transfer process? It is concluded that the compressible energy is transferred locally from the solenoidal part to the compressible part. It is also found that there is an energy cascade of the compressible mode for high turbulent Mach number (M(sub t) greater than or equal to 0.5). Since we assume that the compressibility is weak, the magnitude of the compressible (radiative or cascade) transfer is much smaller than that of solenoidal cascade. These results are further confirmed by studying the triadic energy transfer function, the most fundamental building block of the energy transfer.
Bataille, F.↗
On the magnon interaction in haematite. I - Magnon energy of optical mode.
The effect of magnon interaction on the magnon energies of haematite was studied by the use of a recently developed random phase approximation. In this study, the spin Hamiltonian and the magnon energy were written in a power series of (1/S), where S denotes the magnitude of spin. It is known that the expression of magnon energy is rigorous up to the second term of this series. It is found that the optic mode energy is small if the free optic mode energy is small, which is contrary to Herbert's (1969) conclusion. This direct proportionality between the optic mode energy and the free optic mode energy was not confirmed in the higher order terms of 1/S.
Nagai, O.↗
High power densities from high-temperature materials interactions
Thermionic energy converters and metallic-fluid heat pipes are well suited to serve together synergistically. The two operating cycles appear as simple and isolated as their material problems seem forebodingly deceptive and complicated. Simplified equations verify material properties and interactions as primary influences on the operational effectiveness of both. Each experiences flow limitations in thermal emission and vaporization because of temperature restrictions redounding from thermophysicochemical stability considerations. Topics discussed include: (1) successful limitation of alkali-metal corrosion; (2) protection against external hot corrosive gases; (3) coping with external and internal vaporization; (4) controlling interfacial reactions and diffusion; and (5) meeting other thermophysical challenges; expansion matches and creep.
Morris, J. F.↗
Energetic 0-positive precipitation: A significant energy
The interaction of 0(+) ions with the thermosphere and their subsequent history is described. The large scale effects of this precipitation are examined using a global thermospheric circulation model. A mechanism is suggested by which the energetic 0(+) fluxes may be self-sustaining.
Torr, M. R.↗
High power densities from high-temperature material interactions
Thermionic energy conversion (TEC) and metallic-fluid heat pipes (MFHPs), offering unique advantages in terrestrial and space energy processing by virtue of operating on working-fluid vaporization/condensation cycles that accept great thermal power densities at high temperatures, share complex materials problems. Simplified equations are presented that verify and solve such problems, suggesting the possibility of cost-effective applications in the near term for TEC and MFHP devices. Among the problems discussed are: the limitation of alkali-metal corrosion, protection against hot external gases, external and internal vaporization, interfacial reactions and diffusion, expansion coefficient matching, and creep deformation.
Morris, J. F.↗
Studies of orbital Eoetvoes experiments
A direct force-balance technique was analyzed for carrying out the Eoetvoes experiment in space, which is intended to give sufficient sensitivity to allow investigation of the gravitational interactions of energy stored in the weak interaction. The heart of experiment is an exceedingly sensitive dual accelerometer, containing two proof masses constructed of the materials whose Eoetvoes ratio is to be compared. For use in development of the accelerometer, a magnetic microbalance is proposed in which the weight of the proof mass is supported by magnetic forces which vary very slowly with the proof mass position. It is shown that at least two different mechanizations of the magnetic suspension may be feasible.
Chapman, P. K.↗
Empirical description of the hadron-hadron and hadron-nucleus interaction at the accelerator energy range
Taking into account several assumptions, a formula is transformed into two expressions for kaon and baryon plus antibaryon production in proton interaction and for pion production in pion interactions. Combining both formulae, expression are obtained for the spectrum of kaons and baryons plus antibaryons produced in the meson interactions. For analysis of the cosmic ray propagation in the atmosphere in actual fact, instead of the formulae for interactions of protons and mesons with protons, formulae appropriate for interactions with air nuclei was used. Using the method outlined among others by Elias et al. (1980) simple corrections were introduced to the derived expressions to account for the fact that the target is an air nucleus.
Kubiak, G.↗
Displacement damage in silicon due to secondary neutrons, pions, deuterons, and alphas from proton interactions with materials
The enhancement of displacement damage energy deposition due to secondary neutrons, pions, deuterons, and alphas resulting from high energy proton interactions with aluminium and tungsten shielding are examined in this paper.
silicon↗
Effects of high-energy neutrino production and interactions on stars in close X-ray binaries
Limits are discussed that may be placed on binary systems in which a compact partner is a strong source of high-energy particles that produce photons, neutrinos, and other secondary particles in the companion star. The highest energy neutrinos are absorbed deep in the companion and the associated energy deposition may be large enough to affect its structure or lead to its ultimate disruption. This neutrino heating is evaluated, starting with a detailed numerical calculation of the hadronic cascade induced in the atmosphere of the companion star. For some theoretical models, the resulting energy deposition from neutrino absorption may be so great as to disrupt the companion star over a time scale of 10,000-100,000 yr. Even if the energy deposition is smaller, it may still be high enough to alter the system substantially.
Gaisser, T. K.↗
Application of molecular beams to the study of gas surface interactions at low and moderate energies.
Low and moderate energy gas molecule-solid surface interactions, using molecular beams
Trilling, L.↗
Application of molecular beams to the study of gas surface interactions at low and moderate energies
Low and moderate energy gas molecule-solid surface interactions using molecular beams
Falcovitz, J.↗
Mechanisms for Production of the Diffuse Gamma-ray Continuum Radiation
The production of cosmic gamma radiation from Compton interactions with low energy photons, bremsstrahlung interactions, cosmic ray induced neutral pion production, and matter-antimatter annihilation is discussed.
Stecker, F. W.↗
Mechanisms for production of the diffuse gamma-ray continuum radiation
Basic mechanisms involved in the production of cosmic gamma radiation are outlined. They include Compton interactions with low energy protons, bremsstrahlung interactions, cosmic ray induced neutral pion production, and matter-antimatter annihilation. Detailed data are given on diffuse continuum radiation. Comparative data results are given in tables and graphs.
Stecker, F. W.↗
Supernovae and supernova remnants
The basic features and astrophysics of supernovae of types Ia, Ib, and II and of SNRs are discussed, summarizing the results of recent ground-based and space observations obtained at different wavelengths. Typical data are presented in graphs and sample images, and consideration is given to their implications for shock heating by the initial explosion, radioactive energy input, circumstellar interaction, and pulsar energy input. SNRs described include Tycho's remnant, Kepler's remnant, the Cyg loop, Pup A, the Crab Nebula, the Vela and Crab pulsars, and 0540-69.3 in the LMC. The need for high-spatial-resolution IR and X-ray spectra of these objects is indicated.
Chevalier, Roger A.↗