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Cultured cells provide isolated systems for both biochemical and morphological studies. Previous methods of processing cell culture specimens for electron microscopy (EM) have been limited to sectioning either a monolayer or centrifuged cell suspensions which are not morphologically intact. In our improved method, N -butylglycidyl ether is added to cell cultures (2–5 min with agitation) following in situ fixation (3.0% glutaraldehyde in 0.1 M Pipes, pH 7.2, for 20 min, osmium tetraoxide 4% for 20 min). A thin pliable “sheet” of cells floats free from the plastic culture device and can be manipulated (centrifuged or folded) to obtain a vast number of morphologically intact cells for examination. We have examined several cell types (vascular smooth muscle, lung, liver, and endothelial cells) grown in two types of plastic culture flasks (Nunc and Falcon). This new method provides excellent EM morphology, maximizes the number of cells examined, and allows determination of cell orientation since a remnant of the dissolved flask remains loosely bound to the bottom of the cells.

Descriptions are given of the experimental methods used in determining Al-26 and Mn-53 activities and of the possible improvements that can be expected in the near future. The results obtained for the seven lunar core sections where both Al-26 and Mn-53 are measured with good depth definition are discussed. It is then shown how meteoritic impacts and the secondary effects they induce modify the Al-26 and Mn-53 activities in a core. Using a Monte Carlo method, 150 possible depositional histories for a core are generated; from these the resulting activity profiles for both Al-26 and Mn-53 are computed, using several possible SCR energy spectra. These model-generated profiles are then compared with the experimental profiles in the seven cores, and plausible scenarios for the depositional history of each of the cores are tentatively inferred.

Polyamines are essential for cell growth and differentiation. Ornithine decarboxylase (ODC) is the rate-limiting enzyme in polyamine biosynthesis. Acid phosphatases (AP) are lysosomal enzymes that are important in normal intracellular metabolism. Twenty-four-hour variations in these enzymes may be important in understanding the temporal responses of different tissues to various stimuli. The purpose of this study was to examine a variety of tissues for fluctuations in the levels of ODC and AP over a 24-hr period. Significant circadian variations in the amount of ODC activity were observed in all tissues examined. Activity of AP varied with time of day in the liver, kidney, and heart. The highest and lowest measurements of ODC activity were as follows: liver, 81.5 +/- 7.0, 47.9 +/- 4.4; colon, 11.7 +/- 1.2, 3.1 +/- 0.7; stomach 3.1 +/- 0.4, 0.9 +/- 0.1; kidney, 420.9 +/- 0.9, 67.5 +/- 0.8; and heart, 4.7 +/- 1.0, 2.5 +/- 0.2. The highest and lowest measurements of AP activity were as follows: liver 3.8 +/- 0.1, 2.8 +/- 0.1; kidney, 3.4 +/- 0.1, 1.9 +/- 0.1; and heart, 2.6 +/- 0.1, 2.0 +/- 0.1. These findings suggest that rhythmic fluctuations in polyamine biosynthesis and lysosomal enzymes may influence other metabolic pathways differentially throughout 24 hr.

The intensive development of the liquid scintillation counter for the measurement of tritium has come about in response to a need for a sensitive, reliable, and simple counting method for this difficult-to-measure nuclide. A number of groups participated in this development, but the workers at Los Alamos deserve special mention [1, 2]. Our own work [3] has been almost entirely with C14, although the instrument is the same.

Several radionuclides lighter than Ni, with half-life ≥ 2 weeks and rare gas isotopes of He, Ne, Ar, Kr (including 2 × 105 year 81Kr), and Xe have been measured in two samples from the amphoterite Saint-Severin. The concentration of low-energy products 26Al, 22Na, 21Ne, 53,54Mn, and 83Kr are lower than are normally encountered in stone meteorites of this size, whereas the high-energy products 10Be and 38Ar (in the troilite phase) occur in normal concentrations, suggesting that the samples analyzed (from stone D) were situated in a region where the secondary cosmic radiation is only slightly developed. A comparison with calculated production rates indicates that the samples were, on the average, located at about 3–4 cm from the preatmospheric surface of the meteorite. This conclusion is further supported by high 22Ne/21Ne and 78Kr/83Kr ratios as well as the high track density of heavy cosmic radiation (Z> 24) in hypersthene grains from these samples, and the small calculated neutron density. The cosmic-ray exposure age of this meteorite as calculated from the various pairs of nuclides is (11.2 ± 1.0) × 106 years. It is shown that the relative spallation mass yields of Kr depend on the energy spectrum of cosmic rays.

A large number of radionuclides have been measured as a function of depth in lunar rock 10017 and in bulk fines. Data are reported on (10)Be, (22)Na, (26)Al, (36)Cl, (49)V, (53)mn, (54)Mn (55)Fe, (56)Co, (57)Co, and (59)Ni and on upper limits for (46)Sc, (48)V, (51)Cr, and (60)Co. The results for several nuclides show striking evidence of excess surface production attributable to solar flare particles. Data for short-lived species, (56)Co, (57)CO, (54)Mn, (55)Fe, and (22)Na, appear consistent with fluxes from known recent events. Long-lived species demonstrate the existence of solar flare protons and alphas at least for the last 10(5) to 10(6) years, at fluxes comparable to those now observerved.

The Mars Odyssey Gamma-Ray Spectrometer is a suite of three different instruments, a gamma subsystem (GS), a neutron spectrometer, and a high-energy neutron detector, working together to collect data that will permit the mapping of elemental concentrations on the surface of Mars. The instruments are complimentary in that the neutron instruments have greater sensitivity to low amounts of hydrogen, but their signals saturate as the hydrogen content gets high. The hydrogen signal in the GS, on the other hand, does not saturate at high hydrogen contents and is sensitive to small differences in hydrogen content even when hydrogen is very abundant. The hydrogen signal in the neutron instruments and the GS have a different dependence on depth, and thus by combining both data sets we can infer not only the amount of hydrogen, but constrain its distribution with depth. In addition to hydrogen, the GS determines the abundances of several other elements. The instruments, the basis of the technique, and the data processing requirements are described as are some expected applications of the data to scientific problems.

Precise measurements of the half-life of I-129 in three different meteorites and one lunar surface rock are reported. The meteorite source of I-129 was produced by cosmic ray secondary neutron reactions on Te, while the source in lunar materials in spallation on barium and rare earth elements. The Abee, Allende, and Dhajala meteorites were examined, together with the lunar rock 14310. Details of the process used to extract the iodine are provided. The Abee and Allende samples exhibited a production of 0.5 atom/min per gm of Te from the (n,2n) reaction and 0.05 atom/min/gm for the (n,gamma) reaction. The I-129 is concluded to be a viable tool for long-lived cosmogenic nuclide studies. Further work to extend the data to include the constancy of the cosmic ray flux, the meteorite bombardment history, and the cosmic exposure age dating by means of the I-129 and Xe-129 method is indicated.

The discovery of isotopic anomalies in the calcium- and aluminum-rich inclusions of the Allende meteorite has improved our knowledge of the origin of the solar system. Inability to find more inclusions without destroying the meteorite has hampered further study. By using a fourth-generation computed tomographic scanner with modifications to the software only, the interior of heterogeneous materials such as Allende can be nondestructively probed. The regions of material with high and low atomic numbers are displayed quickly. The object can then be cut to obtain for analysis just the areas of interest.

Interstellar flux of gamma rays analyzing ranger borne scintillation spectrometer measurements

The ways in which explosions are identified are largely a matter of secret information. However, we offer the following article as a partial illustration of how convincing the available data can be. We are grateful to the editors of Nucleonics for permission to use the figures and make a summary-review of this article, which appeared in the August 1952 issue of that journal.

The usefulness of the in situ cosmogenic H-3, C-14, and Be-10 produced by spallation of oxygen nuclei in ice, as tracers to determine net accumulation/ablation rates of ice sheets is explored. The application of the in situ H-3 and Be-10 is severely constrained because at deposition, ice contains appreciable amounts of these isotopes from the atmosphere. The case is much more favorable for C-14, which is not carried with wet precipitations; atmospheric C-14 gets mechanically trapped in the ice during deposition. It is pointed out that cosmogenic C-14 would probably exist as (C-14)O in ice. This seems to be supported by the published results of Fireman and Norris (1981). Considering their inherent amounts in the ice and the expected in situ production rates, conditions under which these isotopes can be used to study net accumulation and ablation rates are discussed. Available data on C-14 and Be-10 on polar ice from accumulation and ablation zones is also discussed. It is concluded that H-3 and C-14 should find wide applications in studying ice dynamics and Be-10 in very special circumstances.

The idea that ice and other trapped volatiles exist in permanently shadowed regions near the lunar poles was proposed by Watson, Murray, and Brown (1961). It is reexamined in the present paper, in the light of the vast increase of lunar knowledge. The stability of the traps and the trapping mechanism are verified. Four potential sources of lunar H2O, namely (1) solar wind reduction of Fe in the regolith, (2) H2O-containing meteoroids, (3) cometary impact, and (4) (the least certain) degassing of the interior, can supply amounts of trapped H2O estimated in the range of 10 to the 16th to 10 to the 17th g. Two important destructive mechanisms have been identified: photodissociation of H2O molecules adsorbed on the sunlit surface and sputtering or decomposition of trapped H2O by solar wind particles. The effect of impact gardening is mainly protective. The question of the presence of H2O in the traps remains open; it can be settled by experiment.

The concentrations of Be-10 and Al-26 in quartz crystals extracted from glacially polished granitic surfaces from the Sierra Nevada range are studied. These surfaces are identified with the glacial advance during the Tioga period about 11,000 yr ago. The measurements yield the most accurate estimates to date for the absolute production rates of three nuclides in SiO2 due to cosmic ray nucleons and muons for geomagnetic latitudes 43.8-44.6 N and altitudes 2.1-3.6 km.

Asteroid families and jet streams, searching for regularities and resonances in mean family elements