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Galvin, A. B.

Publications and source records attributed to Galvin, A. B..

49 records · Page 3
All sourcesNASA NTRSDOE OSTI
NASA NTRS1986

Solar wind Fe and CNO measurements in high-speed flows

Solar wind characteristics in driver plasma and coronal hole-associated flow types are analyzed. Measurements of solar wind Fe charge states and densities in well-defined driver plasma and coronal hole-associated high-speed streams, and charge distributions of CNO ions in high speed streams collected with the ultra low energy charge analyzer on ISEE 3 are examined. The Fe-H velocity differences and Fe/H abundance ratios are studied. The data reveal that the driver plasma solar wind has charge states of 15 or 16 with a coronal temperature = 4 x 10 to the 6th K, and the Fe charge states distributions in coronal hole-associated streams = 9 or 10 with a coronal temperature = 1.4 x 10 to the 6th K; the ionization temperature for the CNO group = (1.3 + or - 0.3) x 10 to the 6th K.

Ipavich, F. M.↗
NASA NTRS1986

Energetic particle beams in the plasma sheet boundary layer following substorm expansion - Simultaneous near-earth and distant tail observations

Simultaneous observations of ions and electron beams in the near-earth and deep magnetotail following the onset of substorm are analyzed in terms of the substorm neutral line model. The observations were collected on March 20, 1983 with ISSE 1 and 3. Energy fluxes and intensity-time profiles of protons and electrons are studied. The data reveal that the reconnection at the near-earth neutral line produces ions and electrons for the plasma sheet boundary layer. The maximum electric potential along the neutral line is evaluated.

Scholer, M.↗
NASA NTRS1985

The mean ionic charges of N, Ne, MG, SI and S in solar energetic particle events

The mean ionic charges of nitrogen, neon, magnesium, silicon, and sulfur in solar flare particle events were determined for 12 flares during the time interval from September 1978 to September 1979. The observations were carried out with the MPI/UoMd ULEZEQ Sensor on the ISEE-3 satellite comparing the results with mean charge states established in a hot coronal plasma under equilibrium conditions, different temperatures for different elements are discussed. These range from approx. 2 million K to 7 million K in a single flare. From flare to flare the variation in temperature for each element is less than the variation between different ion species.

Luhn, A.↗
NASA NTRS1985

Temporal variations of the anomalous oxygen component, 1977 - 1984

A survey is of the long term temporal variations of 6.6 to 12 MeV/nucleon anomalous oxygen at 1 AU covering the period 1977 to 1984. This time interval included the recent solar maximum, with the recovery at neutron monitor energies beginning in 1982. During this time interval, 6.6 to 12 MeV/nucleon 0 fluxes decreased by at least a factor of 50, and indeed remained below the instrumental detection threshold after 1979. By late 1984, neutron monitors had recovered to roughly 1979 levels from the 1982 solar maximum, and anomalous O still remained below the detection threshold.

Mason, G. M.↗
NASA NTRS1985

Energetic particle characteristics of magnetotail flux ropes

During the recent ISEE-3 Geotail Mission three events have been identified from the magnetometer data which are consistent with a spacecraft crossing of a magnetotail flux rope. Energetic electron and proton observations obtained by the Max-Planck-Institut/University of Maryland sensor system during two of the possible flux rope events are presented. During one event remote sensing of the flux rope with energetic protons reveals that the flux rope is crossed by the spacecraft from south to north. This allows determination of the bandedness of the magnetic field twist and of the flux rope velocity relative to the spacecraft. A minimal flux rope radius of 3 earth radii is derived. Energetic proton intensity is highest just inside of the flux rope and decreases towards the core. Energetic electrons are streaming tailward near the outer boundary, indicating openness of the field lines, and are isotropic through the inner part of the flux rope.

Scholer, M.↗
NASA NTRS1985

Suprathermal O(+) and H(+) ion behavior during the March 22, 1979 (CDAW 6), substorms

The present investigation has the objective to report on the behavior of energetic (approximately 130 keV) O(+) ions in the earth's plasma sheet, taking into account observations by the ISEE 1 spacecraft during a magnetically active time interval encompassing two major substorms on March 22, 1979. Attention is also given to suprathermal H(+) and He(++) ions. ISEE 1 plasma sheet observations of the proton and alpha particle phase space densities as a function of energy per charge during the time interval 0933-1000 UT on March 22, 1979 are considered along with the proton phase space density versus energy in the energy interval approximately 10 to 70 keV for the selected time periods 0933-1000 UT (presubstorm) and 1230-1243 UT (recovery phase) during the 1055 substorm on March 22, 1979. A table listing the proton energy density for presubstorm and recovery periods is also provided.

Ipavich, F. M.↗
NASA NTRS1984

Characteristics of suprathermal H(+) and He(++) in plasmoids in the distant magnetotail

Rest frame distribution functions were obtained for suprathermal H(+) and He(2+) ions during 20 particle intensity increases that were observed in the distant magnetotail by ISEE-3. All of these increases were characterized by isotropic, approximately 100-keV electrons, preceded by beaming electrons and velocity-dispersed protons distributions whose signatures are typically associated with plasmoids. In each of the plasmoids, both H(+) and He(2+) are found to be convected tailward, with speeds that range from 200 to 1000 km/sec. The acceleration mechanism is found to depend on particle velocity, and it is established that the solar wind is a dominant plasma source. The plasmoids appear to be expanding at about 100 km/sec during their tailward propagation.

Gloeckler, G.↗
NASA NTRS1984

Abundances and spectra of superathermal H(+), He(++) and heavy ions in a fast moving plasma structure (plasmoid) in the distant geotail

An ISEE-3 Geotail Mission sensor has furnished data on a 16-min particle intensity increase in the distant magnetotail from which rest frame distribution functions have been deduced for 3-150 keV/amu H(+), He(++), and ions with a charge state greater than 3. The event was characterized by isotropic electron distributions and is identified as a tailward-moving plasmoid. These suprathermal ions are convected nearly tailward at an average speed of 1000 + or - 50 km/sec and have an energy density of 150 eV/cu cm. A crosstail expansion speed of about 80 km/sec is indicated.

Gloeckler, G.↗
NASA NTRS1984

Energetic (greater than 100 keV) O(+) ions in the plasma sheet

The first measurements of very energetic (112 - 157 keV) O(+) ions in the earth's magnetosphere are presented. The observations were made with the UMd/MPE ULECA sensor on ISEE-1 on 5 March 1981 at geocentric distances approximately 20 R(E) in the earth's magnetotail. During this time period an Energetic Storm Particle event was observed by the nearly identical sensor on the ISEE-3 spacecraft, located approximately 250 R(E) upstream of the earth's magnetosphere. The ISEE-1 sensor observed a similar temporal profile except for several sharp intensity enhancements, corresponding to substorm recoveries during which the plasma sheet engulfed the spacecraft. During these plasma sheet encounters we observe O(+)/H(+) abundance ratios, at approximately 130 kev, as large as 0.35. In between plasma sheet encounters the O(+)/H(+) ratio at this energy is consistent with zero.

Ipavich, F. M.↗
NASA NTRS1984

Solar wind ionization temperatures inferred from the charge state composition of diffuse particle events

Detailed measurements of the charge state composition of energetic heavy ions in the diffuse component are presented for the first time. Spectral characteristics and charge state measurements for 12 diffuse ion events observed upstream of the earth's bow shock are reported. One event is analyzed in order to illustrate the basic assumptions and general techniques involved in the determination of charge state composition from the data. The probable solar wind origin of the seed population of the diffuse component is used together with the charge state composition of these heavy ions to estimate the charge state composition in the concurrent solar wind, and hence to infer the equilibrium coronal temperatures associated with a variety of solar wind flows. The results are compared with predicted solar wind values.

Galvin, A. B.↗
NASA NTRS1983

Iron charge states observed in the solar wind

Solar wind measurements from the ULECA sensor of the Max-Planck-Institut/University of Maryland experiment on ISEE-3 are reported. The low energy section of approx the ULECA sensor selects particles by their energy per charge (over the range 3.6 keV/Q to 30 keV/Q) and simultaneously measures their total energy with two low-noise solid state detectors. Solar wind Fe charge state measurements from three time periods of high speed solar wind occurring during a post-shock flow and a coronal hole-associated high speed stream are presented. Analysis of the post-shock flow solar wind indicates the charge state distributions for Fe were peaked at approx +16, indicative of an unusually high coronal temperature (3,000,000 K). In contrast, the Fe charge state distribution observed in a coronal hole-associated high speed stream peaks at approx -9, indicating a much lower coronal temperature (1,400,000 K). This constitutes the first reported measurements of iron charge states in a coronal hole-associated high speed stream.

Ipavich, F. M.↗
NASA NTRS1980

Composition and energy spectra of low energy ions observed upstream of the earth's bow shock on ISEE-1

The characteristics of eleven locally accelerated particle events in the energy range from 30 to 125 keV/Q observed upstream of the earth's bow shock have been determined, including composition, energy spectra, and intensity versus time profiles. The measurements were made with the Ultra Low Energy Charge Analyzer sensor on ISEE-1. The composition in these events is similar to that of the solar wind, with a He to proton ratio of 8% and a CNO to He ratio of 6%. The composition is reasonably constant only when evaluated at equal energy per charge. The energy spectra cannot be adequately fit by a single power law in energy; an exponential or Maxwellian in energy per charge gives a satisfactory representation of the spectra. The time-intensity profiles of these upstream events show an inverse velocity dispersion, which may provide clues to the responsible acceleration mechanism.

Ipavich, F. M.↗