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At least 1,153 records · Page 64
All sourcesNASA NTRSDOE OSTI
NASA NTRS1971

Uranium-bearing minerals of lunar rock 12013.

The U distribution in rock 12013 was studied by fission track and elemental mapping techniques. Major U-bearing phases are whitlockite, apatite, zircon, and phase beta, which is a Zr-Ti mineral rich in Fe, Nb, Y, REE, and containing up to 3.6% UO2, 4.7% ThO2 and 4.2% PbO. Calculated microprobe ages for phase beta average 4.0 b.y. and are in reasonable agreement with Rb-Sr and K-Ar ages. Phase beta plays a significant role in the U-Th-Pb systematics of rock 12012 and may play a similar role in the model ages of lunar soil.

Haines, E. L.↗
NASA NTRS1971

U-Pb ages for sphene in a contact metamorphic zone.

U-Pb ages have been determined on sphene concentrates from the 2700 my old Giants Range Granite at varying distances from the contact with the 1100 my old Duluth gabbro. As the contact is approached the sphene ages become more discordant and plot along a chord between 1100 and 2700 my on a concordia diagram. The U-Pb ages for sphene in the contact aureole are more resistant to thermal metamorphism than are K-Ar ages for hornblende and biotite. The resistance relative to U-Pb ages for zircon is more difficult to interpret because the zircon U-Pb ages may have become discordant prior to or after 1100 my ago, whereas the U-Pb ages for sphene appear to have had episodic discordance only at 1100 my ago.

Hanson, G. N.↗
NASA NTRS1971

A case for catastrophic early degassing of the earth.

Evidence is given for the occurrence in early earth history of massive escape of volatiles from the interior of the earth to its surface, which must have had catastrophic proportions. The mechanism and time of this event are inferred from the abundances and distribution of volatiles in the atmosphere, hydrosphere and crust, and from meteorite studies, and geophysical and astronomical observations. This event is linked to the melting of the earth during accretion which resulted in the concentration of U, Th, K and Pb in the outermost portion of the earth and in virtually complete expulsion of nonradiogenic Ar, Ne and Kr from its interior.

Fanale, F. P.↗
NASA NTRS1971

Differential thermal analysis and gas release studies of Apollo 11 samples.

The liquidus-solidus behavior of Apollo 11 lunar fines and the evolution characteristics of CO, nitrogen, He, Ne, and Ar were investigated by use of the combined techniques of high-vacuum differential thermal analysis (DTA) and mass spectrometry between 100 and 1500 C. The DTA thermogram has shown that the lunar fines undergo partial melting over a broad range of temperature from about 915 to 1300 C, with a significant initial melting of glassy and crystalline components within the fines at about 1140 C. The lunar material becomes a homogeneous melt at about 1300 C.

Wachi, F. M.↗
NASA NTRS1972

Nuclear composition and energy spectra in the 1969 April 12 solar-particle event.

Measurement of the charge composition for several of the multicharged nuclei and the energy spectra for hydrogen, helium, and medium (6 less than or equal to Z less than or equal to 9) nuclei in the Apr. 12, 1969, solar-particle event. The energy/nucleon spectral shape of the medium nuclei was again the same as that of the helium nuclei, and the ratio of these two species was consistent with the present best average of 58 plus or minus 5. By combining the results obtained here with previous work, improved estimates of the Ne/O and Mg/O values of 0.16 plus or minus 0.03 and 0.056 plus or minus 0.014, respectively, were obtained. Silicon and sulfur abundances relative to O were determined to be 0.208 plus or minus 0.008 plus or minus 0.006, respectively, and 85% confidence upper limits for Ar and Ca relative to O of 0.017 and 0.010 were obtained. Previously, these last four nuclei had only been listed as a group.

Bertsch, D. L.↗
NASA NTRS1972

Enrichment of very heavy nuclei in the composition of solar accelerated particles.

Measurement of the abundances of the nuclei C, N, O, Ne, Mg, Si, Ar, and Ca and the group Cr-Co relative to oxygen from seven solar energetic-particle events in the energy range from about 14 to 61 MeV per nucleon with a solid-state detector telescope on the OGO-5 satellite, 1968-1971. The differential energy spectra of O (14 to 29 MeV per nucleon) and Cr-Co (3 to 61 MeV per nucleon) have a spectral index of about (-3) for a power law in kinetic energy. The relative abundances of C, N, O, and Ne are in excellent agreement with emulsion studies. However, when compared with the solar photospheric and coronal abundances, the OGO-5 measurements show a large enhancement of relative abundances beginning with Si, and extending to the Cr-Co group. The enhancement over the solar and universal abundances is in rough agreement with the composition of the galactic cosmic radiation.

Mogro-Campero, A.↗
NASA NTRS1972

Quenching of the B /super 2/Sigma-plus state of the CN radical.

The quenching of the B (super 2)Sigma-plus fluorescence from the CN radical has been studied as a function of the relative velocity of the quenching collision and the total pressure in the fluorescence cell. The rate constant for the quenching of the CN fragment by ICN vapor was found to be directly proportional to the relative velocity of the quenching collision. Electronic quenching was also observed for methane, diatomic hydrogen, Kr, and Ar.

Jackson, W. M.↗
NASA NTRS1972

Rare gas record in the largest Apollo 15 rock.

The results obtained from mass-spectrometry analyses of the noble gases He, Ne, Ar, Kr, and Xe in a 182-mg chip of the largest Apollo 15 rock 15555 are presented. The spallation krypton data indicate a well-shielded location through most of the time during which the rock was exposed to cosmic rays. Gas retention ages are estimated. No evidence for the presence of products from plutonium-244 or iodine-129 was found.

Marti, K.↗
NASA NTRS1972

Gas-retention and cosmic-ray exposure ages of lunar rock 15555.

Conclusions are presented regarding the age of formation and exposure to cosmic rays of rock 15555 (a large rock from near the rim of Hadley Rille presumed to be a fragment of the local bedrock), based on isotopic dilution K/Ar and Ar-40/Ar-39 methods. Comparisons are made with other investigators' findings, and some cases of agreement and divergence are discussed.

Podosek, F. A.↗
NASA NTRS1972

Rocket spectroscopy of zeta Orionis.

Analysis of a spectrum of zeta Ori extending from 922 to 1453 A with approximately 0.8 A resolution recorded at rocket altitudes. All lines used in existing models of stellar atmospheres appear in the recorded spectrum with the exception of those masked by telluric N2 or strong P Cygni-type profiles and by an O V line at 1371.29 A. Fifteen multiplets of subordinate lines have been reliably identified, indicating an approximate range of excitation from 0 to 50 eV. Transitions in C III (1176 A), N III (991 A), N V (1239, 1243 A), O VI (1032, 1038 A), Si IV (1394, 1403 A), S IV (1063, 1074 A), and S VI (933, 944 A) have been observed as P Cygni-type profiles presumably arising in a circumstellar envelope. The degree of ionization, transitions present, and mean radial velocities are all consistent with viewing the envelope as a hot (about 100,000 K), rarefied plasma in which collisional ionization is important. Interstellar lines in C I (1277, 1280 A), C II (1036, 1334 A), N I (1134-1135 A), N I (1200-1201 A), N II (1084-1086 A), O I (1302, 1305 A), Si II (1190, 1193 A), Si II (1260 A), and Si II (1304 A) have been definitely identified. Other transitions in Ar II, S I, C I, and Fe II are tentatively identified. The equivalent width of the L alpha line is found to be 10.4 plus or minus 1.6 A, corresponding to a columnar density of 2.0 plus or minus 0.7 x 10 to the 20th per cu cm.

Smith, A. M.↗
NASA NTRS1972

Inert gases in twelve particles and one 'dust' sample from Luna 16.

The inert gases were measured mass-spectrometrically in 12 fragments and one dust sample from Luna 16. The fragments were classified petrologically by microscopic inspection. The major petrologic types were breccias and basalts. The He-4/Ne-20 ratio of the breccias (average 49) was systematically smaller than that of the basalts (average 78), probably because of He-Ne fractionation during or after the formation of the breccias. We suggest that the He-4/Ne-20 ratios of bulk fines in general may reflect the proportions of basaltic and breccia (plus cindery glasses) fragments in the fines. Exposure ages of four fragments are several hundred million years. The Ar-40/Ar-36 slopes of breccias and basalts are identical: 0.65.

Heymann, D.↗
NASA NTRS1972

Rare gas studies of the galactic cosmic ray irradiation history of lunar rocks.

Average irradiation depths and exposure ages of Tranquillity Base rocks are computed on the basis of eight analyses of the five noble gases in whole rock samples and lunar separates from lunar rocks, in conjunction with available literature data. Correlated variations in He-3/Ne-21 and Ar-38/Ne-21 reflect shielding differences. This correlation cannot be explained by diffusion losses, even though evidence for gas loss is obtained from mineral separate data. A qualitative shielding sequence is constructed which agrees reasonably well with the sequence based on Gd isotopic data.

Huneke, J. C.↗
NASA NTRS1972

Foreign-gas broadening of nitrous oxide absorption lines.

We have measured the foreign-gas broadening coefficients for collisional broadening of lines in the nu-3 fundamental of N2O by He, Ne, Ar, Kr, Xe, H2, D2, and CH4. These coefficients, which give the ratio of the line-broadening ability of these gases to the line-broadening ability of N2, can be used with recent measurements and calculations of N2 broadening to obtain optical collision cross sections.

Tubbs, L. D.↗
NASA NTRS1972

LEED structures due to interaction of CO and O2 with /0001/ and /1,0,-1,0/ Re at 20 C to 920 C.

Clean Re surfaces were produced by the Ar(+) ion bombardment technique. Results reported previously by Farnsworth and Zehner (1969) for the adsorption of CO and molecular oxygen on the (0001) Re surface were confirmed. The exposure of a (0001) Re surface to CO at elevated crystal temperatures produced no additional structures. Neither increased surface defect densities nor excitation of the adsorbate enhanced the adsorption characteristics of CO or molecular oxygen on the surfaces studied.

Zehner, D. M.↗
NASA NTRS1972

U-Th-Pb systematics in three Apollo 14 basalts and the problem of initial Pb in lunar rocks.

The isotopic composition of Pb and the elemental concentration of U, Th and Pb were measured on 'total' rock samples 14053, 14073 and 14310 and on mineral separates of 14310 and 14053. These are the first Pb-U isochrons obtained for lunar basalts and indicate a reasonable solution to the previous discrepancy between the different methods of 'absolute' age determination. The resulting U-Pb isochron ages are compatible with the Rb-Sr and K-Ar ages on the same rocks. However, it is not possible to establish a precise time of 'crystallization' from the Pb-U data because of the small angle of intersection between the linear arrays and the concordia curve. These data show that total rock model ages do not in general yield crystallization ages. The data on 14310 and 14053 show that these rocks were formed containing a highly radiogenic initial lead which accounts for the excessively high total rock model ages by the U-Th-Pb method. The data prove that at the time of extrusion of some basalts, unsupported lead with extremely high Pb-207/Pb-206 ratios was added to the lunar surface.

Tera, F.↗
NASA NTRS1972

Numerical calculation of transonic flow about swept wings.

Description of a mixed elliptic-hyperbolic relaxation algorithm which calculates solutions to the three-dimensional, nonlinear transonic small disturbance potential equation for flows about thin swept lifting wings with free-stream Mach number less than 1. The algorithm is designed to treat supercritical flows, including cases with embedded shock waves. Nonrectangular planform shapes, including sweep and taper, are treated by a coordinate transformation which maps the wing planform into a rectangle. Computed results at angles of attack of 0 and 2 deg for a AR = 4, constant chord, 23.75 deg sweptback planform model with a Lockheed C141 airfoil section are compared with data obtained experimentally for both subcritical and supercritical flows. Subcritical results are also compared with those obtained by a subsonic 'panel' method.

Ballhaus, W. F.↗
NASA NTRS1972

Rotational excitation of a rigid rotor - Comparison of two approximate classical models with exact classical results.

A rigid body model and a perturbation technique are used to measure the rotational excitation of a rigid rotor in the determination of the moments of fractional rotational energy transfer in the Ar-N2 system. A table of data is included to compare the obtained results with exact results, showing the failure of the perturbation model to yield correct results.

Labudde, R. A.↗
NASA NTRS1972

Composition and energy spectra of heavy nuclei with 0.5 less than E less than 40 MeV per nucleon in the 1971 January 24 and September 1 solar flares.

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.

Crawford, H. J.↗