Engineering topics
Publications and source records attributed to Cline, T. L..
Observations of a quiet-time interplanetary electron component in the 20 keV to 2 MeV energy range are reported. The measurements fill in the gap between the highest-energy known solar wind and the lowest-energy previously observed electron populations, and connect for the first time the entire solar-quiet interplanetary electron spectrum over a dynamic range of nearly 10 to the 12th power in energy.
Detailed differential energy spectra from gamma ray bursts obtained by IMP-6 are presented. Observations cover times of occurance, photon flux, and temporal and spectral characteristics.
Observation of a quiet-time component of interplanetary electrons having energies above solar-wind energies and below those characterized as cosmic radiation. The energy spectrum of this component generally falls with energy from 18 keV to 1.8 MeV, but shows a feature in the 100 to 300-keV range. The observed temporal variations of the intensity suggest that the 18 to 100-keV portion is solar and that the 0.3 to 1.8-MeV portion is galactic in origin. Solar and terrestrial neutron-decay electrons appear inadequate to explain the 100 to 300-keV feature.
The suggestion by Lin et al. (1972) that a distinct spectral feature exists at about 200 keV, which could be due to a neutron-decay electron component of either solar or galactic origin, is examined. Alternative sources models, including production by nearby galactic objects or acceleration at the outer boundary of the solar system, are also considered.
A quiet time component of interplanetary electrons having energies above solar wind energies and below those characterized as cosmic radiation was observed. Its energy spectrum falls with energy from 18 keV to 1.8 MeV, but it shows a feature in the 100 to 300 keV range. The observed temporal variations of the intensity suggest that the 18 to 100 keV portion is solar and the 0.3 to 1.8 MeV portion is galactic in origin. Solar and terrestrial neutron decay electrons appear inadequate to explain the 100 to 300 keV feature.
Detailed examination of the intensity variations of 3- to 12-MeV interplanetary electrons. The data are from the Goddard cosmic-ray experiment on the Imp satellites and cover the period from just before the last solar minimum through the onset of the present solar maximum (i.e., from December 1963 through August 1969). A morphology for the intensity changes is tentatively proposed that includes solar-flare-associated events, solar co-rotating increases, Forbush decreases, quiet-time increases, and the long-term 11-year variation. It is contended that the electron components observed both during quiescent times and during quiet-time increases are galactic in origin. The quiet-time increases represent a completely new phenomenon that appears to be unique to the low-energy electron population. During a quiet-time increase the electron intensity is enhanced by a factor of 3 to 5 over a period of days, and, in general, these periods anticorrelate with low-energy solar particle events. Qualitatively, their amplitude diminishes with increasing solar activity.
A detailed examination is made of the intensity variations of 3 - 12 MeV interplanetary electrons. The data used are from the cosmic ray experiment flown on the IMP solar minimum through to the onset of the present solar maximum (i.e., from December 1963 through August 1969). A morphology for the intensity changes is tentatively proposed which includes solar flare-associated events, solar co-rotating increases, Forbush decreases, and quiet-time increases, as well as the long term eleven-year variation. It is contended that the electron component observed both during quiescent times and during quiet-time increases are galactic in origin. The quiet-time increases represent a completely new phenomenon that appears to be unique to the low energy electron population. During a quiet-time increase the electron intensity is enhanced by a factor of 3 to 5 over a period of days, and, in general, these periods anti-correlate with low-energy solar particle events. Qualitatively, their amplitude diminishes with increasing solar activity.
Time variations of the 3-12 MeV interplanetary electron intensity, observed by the Explorer-18, -28, and -33 spacecrafts, have been studied in detail. Apart from solar flare effects, there are five distinct periods when the electron intensity has undergone a series of increases, and these are strongly correlated with solar rotation. The intensity increases are separate phenomena, and are strikingly anticorrelated with increases in the low energy solar proton intensity. The electron energy spectrum during those quiet-time increases is typically represented by dJ/dE = k E/2.0 + or - 0.25 similar to the galactic electron spectrum. There are, in addition, Forbush decreases in the electron intensity frequently coincident with those in the neutron monitor. It is concluded that these characteristics all support the hypothesis of a galactic origin for the electrons observed during quiet-time increases.
Characteristics of energetic interplanetary particles and X rays produced by solar activity
Cosmic ray electron and positron differential energy spectra during solar quiet times from OGO- 5 satellite observations in interplanetary space
Quiet time intensity increases and long term solar modulation of interplanetary low energy electrons, using IMP observations
Interplanetary cosmic ray positrons energy spectral component with origin different from interstellar mesons decay
Cosmic ray positrons and negatrons differential intensities near north geomagnetic pole from balloon flight measurements, noting solar modulation effects
Relativistic electron and positron intensity distributions in interplanetary regions
Solar flare delayed relativistic electron appearance, comparing radio, optical and X ray data for particle intensities
OGO-E obtained differential energy spectra of electrons and positrons in interplanetary space
Time variation of 4 to 12 MeV interplanetary electron density in cosmic radiation
Satellite detection of interplanetary positrons with higher intensity than cosmic ray meson production