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At least 937 records · Page 52
All sourcesNASA NTRSDOE OSTI
NASA NTRS1973

Recursive formulas for the partial fraction expansion of a rational function with multiple poles.

The coefficients in the partial fraction expansion considered are given by Heaviside's formula. The evaluation of the coefficients involves the differential of a quotient of two polynomials. A simplified approach for the evaluation of the coefficients is discussed. Leibniz rule is applied and a recurrence formula is derived. A coefficient can also be determined from a system of simultaneous equations. Practical methods for the performance of the computational operations involved in both approaches are considered.

Chang, F.-C.↗
NASA NTRS1973

Angular distributions and polarization fractions of helium resonance radiation (n 1P - 1 1S) in the extreme ultraviolet

Angular intensity distributions of helium (n 1P - 1 1S) resonance photons with respect to the exciting electron beam are presented. The angular intensity distributions were measured at selected electron impact energies from 25 eV (near threshold) to 150 eV. Polarization fractions (Pi) were obtained by analyzing the data in terms of the theoretical relation between angular intensity distribution and Pi, i.e. Iota (theta) = Iota (90) (1 - Pi sq cos theta). The experimental values for Pi are compared with recent theoretical results and with previous experimental values for the (3 1P - 2 1S) transition.

Mumma, M. J.↗
NASA NTRS1974

On the fractional weight of distinct binary n-tuples

It is shown that the fraction p of ones in the Mn positions of M distinct binary n-tuples satisfies a given inequality. This inequality, which simplifies the derivation of the distance property of the Justesen codes, is proved using an elegant information-theoretic argument due to Kriz.

Massey, J. L.↗
NASA NTRS1974

Fractionation of moderately volatile elements in ordinary chondrites

The CI chondrites are the most volatile-rich meteorites. Relative to the CI chondrites, the ordinary chondrites have lower abundances of refractory and volatile elements. Four types of fractionations are summarized in a table. Ordinary-chondrite/CI abundance ratios for moderately volatile elements in H- and L-group chondrites are presented in a graph. Possible explanations for the observed relations are considered, giving attention to several processes which could result in the separation of nebular solids and gases.

Wasson, J. T.↗
NASA NTRS1974

Fractional harmonics in a plasma

Theoretical study of plasma nonlinearity effects that cannot be described by modified linear theory, such, for example, as those effects that arise only when a source of disturbances in a plasma reaches a certain threshold amplitude. In particular, the possibility of fractional harmonic generation, independently of the requirements of the plasma wave decay, is investigated.

Lewak, G. J.↗
NASA NTRS1974

Study of isotopic composition of helium in the fine fraction of Luna 16 lunar surface material

The content of He isotopes is measured in two samples of the lunar surface material returned by the Luna 16 automatic station. Both samples consist of a fine fraction of lunar surface material and were samples from zone A (sample 3-2k) and from zone V (sample 9-1r). The value of He4/He3 and the concentration of the He isotopes are identical for both samples, within the limits of experimental error.

Boltenkov, B. S.↗
NASA NTRS1974

Chemical fractionation in the solar nebula

The sequence of condensation of minerals from a cooling gas of solar composition has been calculated from thermodynamic data assuming complete chemical equilibrium is maintained. The results suggest that the Ca-Al-rich inclusions in Allende and other carbonaceous chondrites are aggregates of the highest temperature condensates. Complete condensation of these elements is followed 100 deg later, by the onset of the crystallization of nickel-iron, forsterite and enstatite. Transport of Ca-Al-rich refractory condensates from one part of the nebula to another before the condensation of these lower-temperature phases may have been responsible for the refractory element fractionations between the different classes of chondrites and possibly for the inferred refractory element enrichment of the moon.

Grossman, L.↗
NASA NTRS1974

Provenance of KREEP and the exotic component - Elemental and isotopic studies of grain size fractions in lunar soils

Sieve fraction analyses of lunar soils reveal the presence of a fine-grained exotic component enriched in K, Rb, Sr, Ba, and in radiogenic Sr in all soils. The probable source of this exotic component is the areas of high-surficial radioactivity observed by orbital gamma ray spectrometry, such as those at Fra Mauro and Archimedes. If the exotic component is fine-grained KREEP, the origin and distribution of KREEP fragments in the soils are identified. It is suggested that the exotic component represents trace element enriched material located at some depth in the Imbrium area which was surficially deposited during Imbrium excavation.

Evensen, N. M.↗
NASA NTRS1977

Fraction collector for electrophoresis

Rotating-tube electrophoresis apparatus employs rotating jet of eluting buffer to reduce effects of convection during separation. Designed for separation of microorganisms and biological species, system combines gravity/gradient compensating of lumen with buffer flush at fraction outlet to increase separation efficiency.

Bier, M.↗
NASA NTRS1975

Chemical fractionation of the lunar regolith by impact melting

Impact-produced agglutinitic glass in both lunar highland and mare soils is enriched in mafic elements, in potassium, phosphorus, and sulfur, and in most lithophile elements, whereas it is depleted in plagioclase components including europium. It is proposed that the chemical fractionation is the result of a multistage partial-melting mechanism that accompanies micrometeoroid impacts into soils. The process would be expected to occur on solar system bodies that have an impact-produced regolith.

Adams, J. B.↗
NASA NTRS1976

Evolution of major mineral compositions and trace element abundances during fractional crystallization of a model lunar composition

The evolution of major mineral compositions and trace element abundances during perfect fractional crystallization of a model lunar magma ocean was calculated. The minerals in the model lunar composition were olivine, orthopyroxene, clinopyroxene, and plagioclase. Lunar bulk composition data, major mineral/melt equilibria data, and trace element partition data were taken from published sources. The results show olivine beginning to crystallize at 1380 C. Approximately 50% of the system crystallizes as olivine. From 50 to 60% solidification, orthopyroxene crystallizes alone. During the final 40% solidification, Ca-rich clinopyroxene and plagioclase crystallize together. Various changes in composition of all these minerals are also noted during the process. Concomitant evolution of major element abundances in the melt is followed along with that of trace element abundances. Consequences of the results for constraints on some aspects of the composition of the lunar magma ocean and of the primitive moon are discussed.

Drake, M. J.↗
NASA NTRS1976

The fast decoding of Reed-Solomon codes using fermat theoretic transforms and continued fractions

It is shown that Reed-Solomon (RS) codes can be decoded by using a fast Fourier transform algorithm over finite fields GF(F sub n) where F sub n is a Fermat prime, and continued fractions. This new transform decoding method is simpler than the standard method for RS codes. The computing time of this new decoding algorithm in software can be faster than the standard decoding method for RS codes.

Welch, L. R.↗
NASA NTRS1976

Drive tube 60009 - A chemical study of magnetic separates of size fractions from five strata

Each bulk soil and both the magnetic and nonmagnetic components of the 90-150 micron and below 20 micron fractions of five soils from drive tube 60009 were analyzed. Samples were analyzed for FeO, Na2O, Sc, Cr, Co, Ni, Hf, Ta, Th, La, Ce, Sm, Eu, Tb, Yb, and Lu by neutron activation analysis. Several samples were fused and analyzed for major elements by electron microprobe analysis. Compositional variations are not systematically related to depth. The compositions of the five soils studied are well explained by a two-component mixing model whose end members are a submature Apollo 16-type soil and an extremely immature anorthositic material similar to 60025. There is evidence that the anorthositic component had received a small amount of exposure before these soils were mixed. After mixing, the soils received little exposure suggesting mixing and deposition on a rapid time scale.

Blanchard, D. P.↗
NASA NTRS1976

Zr-Hf fractionation in chemically defined lunar rock groups

Zirconium and hafnium, a geochemically coherent pair of elements, are strongly fractionated in lunar rocks, as evidenced by a wide range of Zr/Hf mass ratios from 12 for the anorthosite 60015,65A to 50 for the KREEP breccia 14321. This may be explained in part by selective reduction of Zr(4+) to Zr(3+) and exclusion of the Zr(3+) from early crystallized Fe-Ti minerals.

Garg, A. N.↗
NASA NTRS1977

Isotope ratios and chemical fractionation of CO in Lynds 134

A radio observation of (C-12)(O-17) in the dust cloud Lynds 134 is reported, and the question of the (C-13)(O-16)/(C-12)(O-18) ratio across this cloud is considered. A value of approximately 0.28 is obtained for the (C-12)(O-17) column-density ratio, and it is shown that the (C-13)(O-16)/(C-12)(O-18) ratio is very different at two positions in the cloud separated by about 3.75 arcmin. (C-13)(O-16)/(C-12)(O-18) column-density ratios are calculated on the assumption of LTE and found to have a mean value of 4.8 at six positions in the most obscured part of the cloud; the same ratio is determined to be much larger and variable outside the cloud core. It is suggested that chemical fractionation of CO is occurring in this cloud, that (C-13)(O-16) is considerably enriched in its outer regions, and that the cloud's C-12/C-13 ratio is approximately 104.

Dickman, R. L.↗
NASA NTRS1977

Mass fractionation of the lunar surface by solar wind sputtering

An investigation is conducted concerning the mass-fractionation effects produced in connection with the bombardment of the moon by the solar wind. Most of the material ejected by sputtering escapes the moon's gravity, but some returning matter settles back onto the lunar surface. This material, which is somewhat richer in heavier atoms than the starting surface, is incorporated into the heavily radiation-damaged outer surfaces of grains. The investigation indicates that sputtering of the lunar surface by the solar wind will give rise to significant surface heavy atom enrichments if the grain surfaces are allowed to come into sputtering equilibrium.

Switkowski, Z. E.↗
NASA NTRS1977

Chemical fractionation in the solar nebula

The sequence of condensation of minerals from a cooling gas of solar composition has been calculated from thermodynamic data over the pressure range 0.001-0.00001 atm, assuming that complete chemical equilibrium is maintained. The results suggest that the Ca-Al-rich inclusions Allende and other carbonaceous chondrites are aggregates of the highest temperature condensates. Complete condensation of these elements is followed, 100 deg later, by the onset of the crystallization of nickel-iron, forsterite and enstatite. Transport of Ca-Al-rich refractory condensates from one part of the nebula to another before the condensation of these lower-temperature phases may have been responsible for the refractory element fractionations between the different classes of chondrites and possibly for the inferred refractory element enrichment of the Moon. The temperature gap between the condensation temperatures of nickel-iron and forsterite increases with increasing total pressure. Because pressure and temperature probably increased with decreasing heliocentric distance in the solar nebula, Mercury may have accreted from a condensate assemblage having a higher metal/silicate ratio than Venus or Earth which may, in turn, have formed from less oxidized material than Mars.

Grossman, L.↗