Primary cosmic-ray positrons and negatrons in 1968 at energies between 11 and 204 MeV
Cosmic ray positrons and negatron spectra between 11 and 204 MeV
Rice, C. J.↗
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Steady-state flux of positrons and the age of the galactic halo
Electron and positron flux steady state in interstellar space relationship to differential energy spectrum exponent in cosmic rays, discussing galactic halo and age
Brunstein, K.↗
Low-energy cosmic ray positrons and 0.51-Mev gamma rays from the Galaxy
Low energy positrons and gamma rays from large fluxes of galactic cosmic rays
Misra, D.↗
Cosmic ray electrons and positrons of energies 2 to 9.5 MeV observed in interplanetary space
Cosmic ray electron and positron differential energy spectra during solar quiet times from OGO- 5 satellite observations in interplanetary space
Cline, T. L.↗
Interplanetary positrons near 1 MeV from other than the pion to muon to electron process
Interplanetary cosmic ray positrons energy spectral component with origin different from interstellar mesons decay
Cline, T. L.↗
Low-energy cosmic ray positrons and 0.51 MeV gamma rays from the galaxy
Galactic low energy cosmic ray positrons and gamma rays, considering production mechanism in interstellar space
Misra, D.↗
Cosmic-ray negatron and positron spectra observed near Fort Churchill in 1968
Cosmic ray positrons and negatrons differential energy spectra and solar modulation, using balloon-borne magnetic spectrometer
Beuermann, K. P.↗
The electron /negatron and positron/ component of the cosmic radiation
Energy spectrum of primary cosmic ray electrons /negatron and positron/ in interstellar region observed near 1965 solar minimum
Verma, S. D.↗
Cosmic ray positrons and negatrons of energies 10 to 250 MeV at 85 deg geomagnetic latitude
Cosmic ray positrons and negatrons differential intensities near north geomagnetic pole from balloon flight measurements, noting solar modulation effects
Cline, T. L.↗
Relativistic interplanetary electrons and positrons
Relativistic electron and positron intensity distributions in interplanetary regions
Cline, T. L.↗
Positron annihilation rates in lanthanum hydrides
Positron annihilation rates in lanthanum hydrides of various composition
Bos, W. G.↗
Generalized Hylleraas calculation of positron-hydrogen scattering
Positron-hydrogen scattering below positronium pickup threshold by Hylleraas bound technique, discussing phase shifts and linear parameters
Bhatia, A. K.↗
Positron-atom scattering by the Kohn and Harris methods
S wave scattering from H and He positron systems at low energies, applying Kohn and Harris variational methods
Drachman, R. J.↗
Positron annihilation radiation from neutron stars
Balloon observations of a low energy flux line at 2 x 0.001 photons cm/2 s/1 from the galactic center region around 470 keV are interpreted as the positron annihilation radiation that occurs on the surface of old neutron stars and is redshifted by their gravitational fields. An astrophysical model is formulated to explain the observed flux that provides for about 0.2 neutron stars per 3 x 10 to the 49th power cubic meters assuming that the disk thickness is about 1.5 x 10 to the 19th power meters.
Borner, G. A.↗
Phase dependence of positron annihilation in tristearin.
Positron lifetime measurements have been used to investigate the polymorphism of tristearin. The results show that both positronium formation and annihilation are sensitive to the phase changes in tristearin.
Walker, W. W.↗
Positron-annihilation radiation from neutron stars.
Matter accreted on the surfaces of neutron stars consists of energetic particles of a few tens to one or two hundred MeV per nucleon, depending on the neutron-star mass. In addition to heat, such particles produce nuclear reactions with the surface material. It is proposed that the recently observed 473 plus or minus 30 keV spectral feature from the galactic center is gravitationally redshifted positron-annihilation radiation produced at the surfaces of neutron stars. The principal observational tests of the model would be the detection of nuclear gamma-ray lines from the galactic center.
Ramaty, R.↗
The scattering of low energy positrons by helium
Kohn's variational method is used to calculate the positron-helium scattering length and low energy S-wave phase shifts for a quite realistic Hylleraas type of helium function containing an electron-electron correlation term. The zero energy wavefunction is used to calculate the value of the annihilation rate parameter Z sub eff. All the results are significantly different from those for Drachman's helium model B, but are in better agreement with the available experimental data.
Humberston, J. W.↗
Rigorous precision p-wave positron-hydrogen scattering calculation
Rigorous lower-bound p-wave positron-hydrogen phase shifts are calculated below the positronium pickup threshold. The wave function is expanded in terms of the two linearly independent D functions each multiplied by an associated Hilleraas-type radial function with two parameters. Adiabatic and nonadiabatic corrections have been included. The results are found to be larger than Armstead's (1968) in all cases near the upper edge of his estimated uncertainty.
Bhatia, A. K.↗