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Search indexed NASA NTRS and DOE OSTI research on propulsion, heat transfer, battery materials and energy systems. Follow report and document links to the original sources.
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Severe storm mass and energy convective transport characteristics, using ATS-3 cloud photographs and three layer model
Spherical harmonic analysis of worldwide cosmic ray variations during geomagnetic storms, using ground station and satellite data
Type 3 solar radio burst storms at low frequencies, suggesting electron packet exciters propagating with little deceleration
Superthermal electrons continuous stream release into interplanetary medium during hectometric solar noise storm activities
Low latitude DS ionospheric current component and auroral electrojet intensity for intense geomagnetic storms, considering particle observations by ATS 5 synchronous satellite
Type 3 solar LF radio burst storms, considering streamer density, inhomogeneities and solar wind speed
Turbopause oxygen/nitrogen decrease effect on ion and neutral composition changes in thermospheric region during magnetic storm, using simultaneous ionospheric and atmospheric equations
Relativistic electron precipitation during magnetic storms, showing cyclotron resonances with electromagnetic ion cyclotron waves
Thermospheric winds measurement during geomagnetic storms with Fabry-Perot interferometer from Doppler shift of two 6300 A fringe profiles
Plasmaspheric ambient hydrogen and helium atomic cations density measurement by OGO 5 ion mass spectrometer during magnetic storm, noting relationship to auroral red arcs
Electron content spatial and temporal variation during ionospheric storm of 8 March 1970 after total solar eclipse
Explorer 12 magnetic field observations of magnetopause current layer during magnetic storm, interpreting data by magnetosphere model
Mineralogy, chemistry and origin of KREEP /potassium, rare earth element and phosphorus/ component in Apollo 12 soil and breccia samples from Ocean of Storms
Pyroxenes and olivines in lunar rocks from Ocean of Storms, observing plastic deformational processes since crystallization by optical, X ray and electron microprobes
The role of jet streams in the development of severe storms was analyzed. Local variations of flow resulting from rapid changes of geostrophic velocity along the air trajectory or inertial instability can produce cold advection. An analysis of meso-network data for 1968 and 1969 was performed. Although inertial instability was present in the network, local deviations in wind direction and cold advection were not detected.
Simultaneous observations are presented from the S3-A (Explorer 45) satellite of the magnetic signature of the ring current and complete measurements of the proton ring current to distances of 5.24 R sub E during the double magnetic storm of 16 to 19 December 1971.
Relativistic electrons can have cyclotron resonances with electromagnetic cyclotron waves. The resonant energy is generally well above 1 MeV throughout the magnetosphere, but it can fall to 1 MeV just within the plasmapause. This also corresponds to the region where ring current (10 to 50 keV) protons are expected to be strongly unstable. The resulting ion cyclotron wave amplitudes necessary to precipitate ring current protons leads to electron lifetimes near the strong diffusion limit ( 100 sec). Thus, 1 MeV electrons whose drift orbits intersect the stormtime plasmapause should rapidly be precipitated in the region 3 L 5 during the initial phase of a magnetic storm.
Neutral density data were obtained near 400 km (1600 LT) from a microphone density gage on OGO-6 from 0 to 40 deg N geomagnetic latitude for 25 September through 3 October 1969. Several geomagnetic storms occurred during this period. Least squares fits were made to data points on density scatter diagrams. An equation representing the least squares fit was computed for each delay time. The equation of best fit (and the corresponding time delay between the density and the magnetic index which resulted in this best fit) was found by choosing the equation that gave the minimum standard error. The implications of the time differences associated with the best fits at various latitudes and longitudes are discussed with regard to the time delays involved in geomagnetic heating of the neutral upper atmosphere.