On the effects of monoenergetic electrons in a steady-state, low pressure plasma
Electron scattering effects in beam generated plasma
Milder, N. L.↗
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Radiative interactions of electrons with matter
Equipment and capabilities developed in investigation of K and L shell ionization cross sections, X ray intensity ratios, bremsstrahlung spectrum, coincidence, and inelastic electron scattering
Quarles, C. A.↗
X-ray spectrum of Scorpius X-1 obtained with a Bragg crystal spectrometer
X ray spectrum measurement of Scorpius X-1 by Bragg spectrometer, explaining emission or absorption absence by source model with line weakened by electron scattering
Angel, J. R. P.↗
Radiative transfer in an ionized medium at high temperature
Electron scattering effects on spectral emission at optical and X ray wavelengths for homogeneous spherical ionized hydrogen plasma cloud, discussing radiation transfer
Garmire, G. P.↗
Radiative transfer in an ionized medium at high temperature
Homogeneous spherical hot hydrogen plasma cloud at various temperatures and optical depths, presenting electron scattering effects on optical and X ray spectral emission
Garmire, G. P.↗
Deformed Brueckner-Hartree-Fock calculations
The renormalized Brueckner-Hartree-Fock (RBHF) theory for many-body nuclear systems is generalized to permit calculations for intrinsic states having permanent deformation. Both Hartree-Fock and Brueckner self-consistencies are satisfied, and details of the numerical techniques are discussed. The Hamada-Johnston interaction is used in a study of deformations, binding, size, and separation energies for several nuclei. Electromagnetic transition rates, moments, and electron scattering form factors are calculated using nuclear wave functions obtained by angular momentum projection. Comparison is made to experiment as well as to predictions of ordinary and density-dependent Hartree-Fock Theory.
Ford, W. F.↗
Energy loss of a relativistic ion in a plasma.
The stopping power of a plasma for a relativistic heavy ion is calculated in a simplified derivation. The total contribution results from (1) individual electron scattering in the Coulomb field of the ion wherein large momentum transfers are involved and (2) small momentum transfers in which quantized plasma oscillations are excited. The resulting general formula for the stopping power is in agreement with a specialization of the results of a more elaborate treatment by Tsytovich. The nonrelativistic limit of the general formula agrees with an expression given earlier by Larkin from field-theory techniques and by the author in a Born-approximation approach. However, the general formula differs slightly in its details from that given by Hayakawa and Kitao.
Gould, R. J.↗
The effects of recent opacity corrections on a main-sequence stellar model of 2.25 solar masses.
Comparison of models calculated with the opacities of Carson et al. (1968) and the electron-scattering corrections of Watson with models based on the opacities of Cox et al. (1965). The models have a mass of 2.25 solar masses and a chemical composition with X = 0.596 and Z = 0.02. With the adopted formulas representing the new opacities, it is found that the percentage changes with respect to the model based on the opacities of Cox et al. can be as large as +11 for the stellar radius, -42 for the luminosity, -15 for the effective temperature, -30 for the mass of the convective core, -8 for the central pressure, and -4 for both the central density and the central temperature.
Novotny, E.↗
Yields of gamma rays emitted following capture of negative muons by Si28 and Mg24.
Measurement of the yields of specific final states excited in the capture of negative muons by Mg24 and Si28. The yields are compared with the cross sections for excitation of the analog states by 180 deg electron scattering and with the relative populations of levels produced by the decay of the giant-dipole-resonance states.
Miller, G. H.↗
Linear momentum transfer effects in molecular dissociation produced by electron impact.
In this study of molecular dissociation produced by electron impact, diatomic systems and polyatomic molecules are considered, and attention is given to the effects of thermal motion and of momentum transfer in the collision process. A procedure is described which makes it possible to 'construct' both the laboratory angular distribution and velocity distribution of the atomic fragments (or, alternatively, the time-of-flight distribution). The calculation assumes that s-wave electron scattering predominates, i.e., that excitation occurs near threshold. The computational procedure may also be reversed to allow construction of possible molecular models to fit given experimental angular and velocity distribution data.
Misakian, M.↗
Electron impact excitation and assignment of the low-lying electronic states of CO2
Electron scattering spectra of CO2 are reported in the 7 to 10 eV energy-loss range, at energies of 0.2, 0.35, 0.6, 0.7, and 7.0 eV above threshold, and at a scattering angle of 90 deg. Several new distinct overlapping continua with weak, diffuse bands superimposed are observed to lie in this energy-loss range. The experimental spectra are discussed in the light of recent ab initio configuration-interaction calculations of the vertical transition energies of CO2. The experimental spectra are shown to be consistent with the excitation states of CO2.
Hall, R. I.↗
Deformed Brueckner-Hartree-Fock calculations.
The renormalized Brueckner-Hartree-Fock (RBHF) theory for many-body nuclear systems has been generalized to permit calculations for intrinsic states having permanent deformation. Both Hartree-Fock and Brueckner self-consistencies are satisfied, and details of the numerical techniques are discussed. The Hamada-Johnston interaction is used in a study of deformations, binding, size, and separation energies for several nuclei. Electromagnetic transition rates, moments, and electron scattering form factors are calculated using nuclear wave functions obtained by angular momentum projection. Comparison is made to experiment as well as to predictions of ordinary and density-dependent Hartree-Fock theory.
Ford, W. F.↗
Electron impact excitation and assignment of the low-lying electronic states of N2O
Electron scattering spectra of nitrous oxide are reported in the 5- to 10-eV energy-loss range at scattering angles of 20, 30, 90, and 130 deg at a residual energy of 7.0 eV; and at residual energies of 10.0, 2.0, 1.0, 0.6, and 0.2 eV at a scattering angle of 90 deg. Several new distinct and overlapping continua are observed to lie in this energy-loss range. The experimental spectra are discussed in the light of semiempirical INDO calculations of Chutjian and Segal (1972) of the vertical transition energies of N2O. An assignment of the symmetries of the observed excitations consistent with the experimental and theoretical data is suggested.
Hall, R. I.↗
The nature of Cygnus X-3 - A prototype for old population binary X-ray sources
Description of a model for Cyg X-3 based on a short-lived phase in the evolution of a U Geminorum-type binary where rapid mass transfer and mass loss occurs. X rays are generated by accretion on the white dwarf component, while both stars are enveloped in a thick stellar wind emanating from the red dwarf. Electron scattering in the cloud is responsible for the modulation of the X rays with the orbital period of 4.8 hours. Ultraviolet radiation and low-energy X rays absorbed in the cloud are reradiated in the optical and infrared, which, it is predicted, will display a 4.8-hr modulation in phase with the X-ray light curve. The X-ray absorption cutoff should also vary with phase, appearing at minimum energy when the source is at maximum light. The model also provides a framework in which certain aspects of the associated nonthermal radio source may be understood. Finally, it is suggested that the model may be applicable to Sco X-1 as well.
Davidsen, A.↗
Influence of rotation on the maximum mass of pulsationally stable stars
The critical mass for stability against radial pulsations in rotating, homogeneous main-sequence stars is found to be greater than in the case of no rotation. Analytic and detailed numerical models show that the critical mass rises steeply with increasing concentration of angular momentum to the center of the star. For uniform rotation near breakup velocity at the star's equator the critical mass is about 850 solar masses if an electron-scattering opacity is used, or about 5000 solar masses if the opacities of Cox and Stewart are used. For nonuniform rotation with a constant ratio of centrifugal force to gravity in the star, the critical mass becomes 'infinite' long before breakup velocity is attained. The relevance of the present results to several observational problems is noted.
Stothers, R.↗
Influence of opacity on the pulsational stability of massive stars with uniform chemical composition. II - Modified Kramers opacity
The pulsational stability of massive, chemically homogeneous stars of Population I has been investigated for a range of simple opacity representations consisting of a straight sum of electron-scattering and modified Kramers opacity. The critical mass for stability against nuclear-energized pulsations is found to be extraordinarily sensitive to small changes in the coefficient and/or temperature exponent of the absorption part of the opacity law. A gradual increase in the atomic absorption (dominant near the stellar surface) first raises the critical mass, then restricts the upper mass limit for instability, and finally eliminates pulsational instability at all masses.
Sastri, V. K.↗
High resolution daytime photoelectron energy spectra from AE-E
The daytime photoelectron energy spectrum has been measured at altitudes above 154 km by the photoelectron-spectrometer experiment on the Atmosphere Explorer-E satellite. Below 200 km, well-resolved peaks are observed in the spectrum corresponding to production of O(+) and N2(+) in various electronic states from photoionization of N2 and O by solar He II (304A) radiation. Vibration-rotation excitation of N2 by inelastic electron scattering is observed at 2.5 eV. The features due to nitrogen disappear from the spectrum at altitudes above 200 km.
Doering, J. P.↗
Evidence for a 17-d periodicity from Cyg X-3
Data are presented from the Ariel-V All-Sky Monitor which indicate a 17-day periodicity of the X-ray spectra from Cyg X-3 (3U2030+40). The data are consistent with data from the Ariel V Sky Survey Experiment. Assuming that the high intensity state of Cyg X-3 is well fitted by a structureless black body (Serlemitsos et al., 1975), and that the 17-day maxima correspond to increased electron scattering in the source, it is suggested that the 17-day effect is analogous to the 35-day variation in Her X-1. The possible explanation of this phenomenon as a result of the 17-day orbital period of the binary system containing Cyg X-3 is severely constrained by the stability of the well-known 4.8-hour variation.
Holt, S. S.↗