The composition and origin of the moon     

Don L. Anderson 《Earth and Planetary Science Letters》1973,18(2):301-316

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The depth distribution of hydrogen in lunar materials     

D.A. Leich  T.A. Tombrello  D.S. Burnett 《Earth and Planetary Science Letters》1973,19(3):305-314

A technique employing the resonant nuclear reaction ¹H(¹⁹F, αγ) ¹⁶O has been used to measure hydrogen concentration versus depth in selected coarse fine fragments from the Apollo 11 and Apollo 15 missions, and in glass coated surface chips from two Apollo 15 rocks. The highly variable hydrogen content in the coarse fine fragments is concentrated mainly in a layer extending from the surface to a depth of 2000 ± 500A?. The hydrogen content of the surface region of the Apollo 15 rock chips is comparable to that of the coarse fine samples, but is concentrated mainly within a few hundred angstroms of the surface. The hydrogen depth distribution in a piece of platinum foil from the Apollo 16 Lunar surface Cosmic Ray Experiment was also measured in an attempt to place a limit on the flux of 10–40 keV protons associated with a solar flare event.  相似文献   

VEGETATION PRODUCTIVITY AND THE POTENTIAL POPULATION OF THE CLASSIC MAYA     

Steven L. Driever  B.A.  M.S.  Ph.D.  Don R. Hoy  B.A.  M.A.  Ph.D. 《Singapore journal of tropical geography》1984,5(2):140-153

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The detection of binary companions to subdwarf B stars     

C. Simon Jeffery  & Don L. Pollacco 《Monthly notices of the Royal Astronomical Society》1998,298(1):179-184

Intermediate dispersion spectroscopy of a sample of 40 hot subdwarf B stars between 5500 and 9000Å has been obtained. The sample includes a large fraction of targets which have been studied photometrically. Seven targets show strong lines arising from the infrared Ca  ii triplet, the unequivocal signature of a cool companion. The positive Ca  ii identifications include known photometric binaries and new targets; all are associated with a photometric red excess. Assuming a canonical value for the subdwarf luminosity, all of the detected companions are overluminous compared with the main sequence. The detection procedure indicates an improved and more secure method for the measurement of the binary frequency of hot subdwarfs.  相似文献   

Metal and Bi/Pb microdistribution studies of an L3 chondrite: their implications for a meteorite parent body     

Dorothy S. Woolum  D.S. Burnett 《Geochimica et cosmochimica acta》1981,45(9):1619-1632

We find strong localizations (relative to bulk) of Bi and to a lesser extent Pb. in some of the kamacite grains in Khohar. Other kamacite grains show no such enrichments. There are distinctive and correlated differences in the Ni contents of the two kamacite populations, with the Bi/Pb-rich kamacite grains having consistently lower Ni levels (sometimes unusually low. ~ 2% Ni) than the Bi/Pb-poor kamacite, which typically have ~ 6–7% Ni. The Bi/Pb-rich kamacite grains are also distinguished on the basis of their etching behavior, exhibiting a highly reactive attack, which has not been observed previously and which we believe may be due to the fact that the Bi/Pb-rich kamacite is finely polycrystalline.We conclude that the trace element microdistributions were not established in the nebula. Nor is it likely that the enrichments occurred with slow cooling in the presence of a vapor phase during the kamacite-taenite phase transition. Rather, the Bi/Pb-rich kamacite most likely reflect the occurrence of a brief reheating episode (or episodes), which may have been shock-induced and which was followed by rapid cooling. We find fine-grained metal-sulfide intergrowths which testify to such a reheating event, and one likely candidate for the site of this event is a hot ejecta blanket at the parent body surface. Iron oxides are found in our Khohar sections. We believe that they are not due to terrestrial alteration, that they are magnetite and that the magnetite probably originated in the same dynamic event in which the Bi/Pb distributions were established. The present data do not allow us to confidently determine whether the event occurred prior to, during, or after the compaction of this meteorite, although the simplest interpretation of the data would indicate the first alternative. Bulk Bi data for Khohar has been used for inferring accretion temperatures and this now appears inappropriate.  相似文献   

The impact of drilling fluid and well cuttings on polychaete feeding guilds from the US northeastern continental shelf     

Don Maurer  Wayne Leathem  Charles Menzie 《Marine pollution bulletin》1981,12(10):342-347

The effect of recent drilling operations (fluid and well cuttings) on polychaete feeding guilds from the continental shelf off Atlantic City, New Jersey, was examined. Although there were some adverse effects on macrobenthos from 2160 metric tons of cuttings and mud solids discharged into the marine environment, the composition of polychaete feeding guilds remained essentially unchanged. This key trophic relationship between polychaetes and the changing environment due to the drilling operation was apparently uninterrupted. This relationship remains to be examined in other natural and perturbed habitats.  相似文献   

Boron concentrations in carbonaceous chondrites     

Martha Riherd Weller  Marian Furst  T.A. Tombrello  D.S. Burnett 《Geochimica et cosmochimica acta》1978,42(7):999-1009

We have analyzed B in carbonaceous chondrites in order to clarify a factor of 100 difference between the solar system B abundance derived from the solar photosphere and that inferred from previous meteorite data. Consistent results were obtained from two instrumental methods for B analysis: (a) counting of the high energy betas from ¹²B produced by the ¹¹B(d,p) reaction, and (b) measurement of particle track densities from ¹⁰B(n,α)⁷Li in a plastic track detector affixed to a homogenized meteorite sample. Contamination is a major problem in B analyses, but extensive testing showed that our results were not seriously affected. Our B concentrations are typically 1–2 ppm and are a factor of 2–6 lower than previous carbonaceous chondrite measurements. Our data for the Cl chondrites Ivuna and Orgueil would indicate a solar system B/Si atomic abundance ratio of 58 × 10^?6, but this is still a factor of 2–10 higher than the photospheric estimates. It may be that B is depleted in the sun by thermonuclear processes; however, the similarity of photospheric and meteoritic Be abundances is a problem for this point of view. Alternatively, B may be enhanced in carbonaceous chondrites, but this would make B a cosmochemically unique element. A mm-sized (Fe,Mn,Mg)CO₃ crystal from Orgueil shows no B enrichment. We find ¹⁰B ≤ 10¹⁶ atoms/g in two Allende fine-grained inclusions suggesting that B is not a refractory element under solar nebula conditions. This ¹⁰B limit, when taken as a limit on ¹⁰Be when the inclusion formed, puts constraints on the possibility of a solar system synthesis of ²⁶Al. For a proton spectrum of E^?a, a must be ≥ 3 if a solar gas is irradiated or a ≥1.5 if dust of solar composition is irradiated.  相似文献   

Evolution of Ground-Water Management Policy for Laramie, Wyoming, 1869-1979     

Peter W. Huntoon  Don A. Lundyb 《Ground water》1979,17(5):470-475

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Programmable Hand Calculator Programs for Pumping and Injection Wells: I — Constant or Variable Pumping (Injection) Rate, Single or Multiple Fully Penetrating Wells     

Don L. Warner  M. Gene Yow 《Ground water》1979,17(6):532-537

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Bismuth and ²⁰⁸Pb microdistributions in enstatite chondrites     

Dorothy S. Woolum  D.S. Burnett  L.S. August 《Geochimica et cosmochimica acta》1979,43(11):1819-1828

Polished sections of 5 enstatite chondrites have been irradiated with 30 MeV ⁴He ions to produce the alpha-radioactive nuclei ²¹¹At and ²¹⁰Po from ²⁰⁹Bi and ²⁰⁸Pb, respectively. The distribution of alpha activity can be mapped, using cellulose nitrate as an alpha track detector, to give the corresponding Bi or Pb distributions in the meteorite. No strong localization of Bi or ²⁰⁸Pb was found; relatively uniform track distributions were observed. In particular, metal or sulfide grains are not enriched in Bi or Pb (relative to bulk), which is in agreement with the predictions of nebular condensation calculations. While the track distributions appear uniform, the results of detailed, track-by-track mappings of the Bi detectors indicate that the Bi is not totally randomly distributed; the statistical fluctuations in the observed track density are different for the cases where the Bi is totally randomly distributed and where the Bi is localized in point sources. Assuming that the Bi in a given sample is localized in identical point sources which are uniformly distributed throughout the sample, the observed relative population densities of clusters (‘stars’) of small numbers of tracks (2–5) corresponds to Bi being localized, with ~90% in grains with about 10^?16g-Bi (~3 × 10⁵Biatoms), and with ~10% in 4 × 10^?14 g-Bi sources. If these are elemental Bi, as predicted theoretically, they are ~ 10² Å and 10³ Å in size, respectively.  相似文献