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An impact parameter method using Coulomb trajectories is applied to the calculation of cross sections for two electron detachment processes. The asymptotic behavior of the cross sections at high energies is investigated in detail. Energy distributions of ejected electrons at three different incident energies are also calculated. Some of the results obtained are compared with available experimental data.
Measurement of energy spectra of O, Si, and Fe between 0.5 and 40 MeV per nucleon with stacks of plastic detectors exposed in a rocket during the Jan. 24, 1971 flare. The Fe/Si ratio decreases from 1.8 plus or minus 0.3 to 0.42 plus or minus 0.14 with energy. In both the January 24 flare and the September 1 flare, the abundances of elements 10 less than or equal to Z less than or equal to 28 at approximately 15 MeV per nucleon are similar to high-energy cosmic-ray source abundances; S, Ne, and Ar are significantly lower than current solar values.
A conventional and a tandem bladed stage were designed for a comparative experimental evaluation in a 0.8 hub/tip ratio single-stage compressor. Based on a preliminary design study, a radially constant work input distribution was selected for the rotor designs. Velocity diagrams and blade leading and trailing edge angles selected for the conventional rotor and stator were used in the design of the tandem blading. The effects of axial velocity ratio and secondary flow on turning were included in the selection of blade leading and trailing edge angles. Design values of rotor tip velocity and stage pressure ratio were 757 ft/sec and 1.26, respectively.
Activities and data reported cover experimental design, mechanization onboard the aircraft, survey operations, quick look and automated data reduction, and a qualitative comparison of survey data with predicted values for the radio frequency survey. The survey was designed to measure amplitude, frequency and time of occurrence of terrestrial emissions in the VHF band during overflights of heavily populated metropolitan areas located on the Pacific Coast of the Continental United States by sensing and recording equipment installed in jet aircraft.
Interpretations of photography of Orientale Basin deposits obtained under earthshine illumination conditions during the Apollo 16 mission are presented. Although the quality of these photographs is less than that obtainable in sunshine, these regions are in the dark during Apollo missions because of the locations of the Apollo landing sites. Photography of these regions under different lighting geometry and from different viewpoints is therefore a useful addition to previous photographic data. Oblique photography was obtained of Riccioli Crater and adjacent areas, which lie northeast of the Orientale Basin.
An explanation is presented of the method used to locate the elastic axis and the method to determine the EI and GJ distributions along the elastic axes of wings with a 2-spar (front and rear) construction or a single torque-box construction.
Analyses for Experiment M512, Materials Processing Facility (MSFC), to be used for evaluating the performance of the Skylab corollary experiments under preflight, inflight, and post-flight conditions are presented. Experiment contingency plan workaround procedure and malfunction analyses are presented in order to assist in making the experiment operationally successful.
Preliminary parametric studies were performed to establish size, weight and packaging arrangements for aerodynamic decelerator devices that could be used for recovery of the expended solid propellant rocket motors used in the launch phase of the Space Shuttle System. Computations were made using standard engineering analysis techniques. Terminal stage parachutes were sized to provide equilibrium descent velocities for water entry that are presently thought to be acceptable without developing loads that could exceed the boosters structural integrity. The performance characteristics of the aerodynamic parachute decelerator devices considered are based on analysis and prior test results for similar configurations and are assumed to be maintained at the scale requirements of the present problem.
The contamination control program plan delineates the cleanliness requirements to be attained and maintained, and the methods to be utilized, in the fabrication, handling, test, calibration, shipment, pre-installation checkout and installation for the ultraviolet spectrometer experiment prototype, qualification and flight equipment.
If the outputs of the two channels are spacially registered and combined to generate a third variable which reflects the differences between the two outputs, then this variable can then be redisplayed in image form and its magnitude should be relatable to the silica content of the rocks imaged. Two methods were proposed for generating this third variable, the first is to take the difference in apparent temperature between the two channels and the second is to ratio the voltage outputs of the two channels. The responses of the two channel high resolution surface composition mapping radiometer and the thermal channels of the MSDS scanner were calculated from data recorded with the NASA IR pallet and simulate the output of these systems had they been flying over the same targets as the IR pallet.
A preflight assessment of the Skylab VHF ranging coverage for the rendezvous portion of the nominal SL-1/SL-3 mission is reported, assuming a 27 July 1973 SL-3 launch. Data are based on a nominal attitude trajectory, which has the Saturn workshop in a solar inertial attitude throughout the rendezvous; the CSM terminal phase initiation maneuver is nominal. An addendum to this report is being prepared, which considers the effects of early and late TPI maneuvers. Curves are presented which show the variation in received power levels on both spacecraft-to-spacecraft links from about 600 n.mi. range to CSM and SWS station keeping. Appropriate threshold levels are shown on these received power curves to indicate zero circuit margins for the ranging function.
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In the summer of 1971 new measurements were made of the primary electron spectrum from 1 to 20 GeV with an electron spectrometer telescope at Fort Churchill. This telescope has been calibrated by using electrons and pions of 0.5 to 15 GeV at the Stanford Linear Accelerator in early 1971 and again in 1972. The calibration results suggest that the events observed are due to interactions of high-energy protons. The measured primary electron spectrum is uncomfortably close to that calculated for secondary electrons produced by the interaction of cosmic ray nuclei with interstellar hydrogen in the Galaxy, and therefore the question of the origin of the high-energy electrons is reopened. The problem of the age of cosmic ray electrons must also be reexamined if the measured spectrum is found to extend to still higher energies.
Tracks of 1000 solar particles with charge Z not less than 10 and tracks of about 150 particles with Z equal to 8 have been analyzed in a stack of plastic detectors exposed in a rocket during the solar flare of Jan. 25, 1971. The energy spectra peak at about 1.5 MeV/nuc, with the flux falling to zero at about 0.4 MeV/nuc. Fe, Si, and O appear to have similar energy spectra for energies between 2 and 12 MeV/nuc.
All routine hematological measurements for the Skylab simulation test were within normal astronaut population limits for the CDR, SPT, and PLT, with one exception: A significant lymphopenia was observed in the PLT during the post test period, possibly the reflection of increased adrenal corticoid secretion. No ultrastructural red cell membrane abnormalities were observed in any of the subjects, nor were any red corpuscle morphological abnormalities noted. Slight elevations in the PLT's red corpuscular potassium were observed in the younger corpuscles after chamber entrance and again upon egress. This probably represents newly released young red cells from hematopoietic tissue. Flame photometric analyses confirm the fact that potassium is indeed higher in the younger cells of all subjects examined.