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Balloon observations registering scatter angles in a liquid scintillator have revealed gamma-ray bursts having energies as low as 10 to the -7th ergs per square cm. The burst distribution is graphed according to energy and frequency. The hypothesis that the bursts are galactic in origin is in good agreement with their small recorded energies and their predicted distribution on the graph.
Observations during 1972 from an experiment on OSO 7 detected a 2-10-keV X-ray flux of 1.7 by 10 to the -10th power erg/sq cm per sec from a source coincident with MSH 14-63, the most probable candidate for association with the A.D. 185 supernova. Both the present data and those of Naranan et al. (1977) at lower energy can be fitted by a dual-temperature thermal spectrum similar to that observed in other young supernova remnants. Model calculations indicate that a mass in excess of 5 solar masses must have been ejected in the A.D. 185 supernova event.
The ratio of deuterium to hydrogen in the Jovian atmosphere has been calculated using a new approach. D/C is obtained from weak lines of HD and CH4 in the visible region of the spectrum while C/H is derived from stronger methane and hydrogen absorptions near 1 micron. This technique permits minimization of the varying effects on line formation caused by scattering in the Jovian atmosphere while relying on absorption bands whose strengths have been measured in the laboratory. The result is a deuterium-to-hydrogen ratio of 2.3 + or - 1.1 times 10 to the -5th power, within the range of local interstellar values
The interaction of neutron beams with He-3 gas is of interest for nuclear pumped lasers. The effects of spectral dependence of the neutron beam, neutron attenuation in the gas-filled laser tube, and transport of the charged-particle He-3(n, p)He-3 reaction products are treated in detail. An expression for the energy density as a function of position within the tube, tube radius, operating pressure, and neutron fluence is given. The maximum energy density within the optical cavity is achieved when the tube radius is 3.26/P where P (atm) is the operating pressure. The variation of radius by 50% above and below optimum will change the energy density at most by 10%, although performance degrades quickly for radii outside this range. If the optimum tube radius is used for each operating pressure, then the power density on the centerline (kW/cu cm) is given as 9.3 x 10 to the -18th power times the operating pressure times flux in a thermal neutron environment of flux (n/sq cm sec).
From a comparison of the Mariner 10 third encounter UV spectrometer data with intensities generated from a newly constructed model exosphere, a new value of 4.5 x 10 to the -4th power for the fraction of the solar wind He(++) flux to be intercepted and captured by Mercury's magnetosphere, if the observed He atmosphere is maintained by the solar wind, has been derived. If an internal source for He prevails, the corresponding upper bound for the global outgassing rate is estimated to be 4.5 x 10 to the 22nd power/s. These values differ from those given earlier because of the present use of a surface temperature distribution satisfying the heat equation over Mercury's entire surface which employs Mariner-10-determined mean surface thermal characteristics. The mean standoff distance of Mercury's magnetopause averaged over Mercury's orbit is also used. Agreement between the observed and calculated intensities is found to be good. Minor discrepancies on the nightside of the terminator are explicable in terms of differences between actual and computed temperatures and scale height structure changes.
All 23 stable rare gas isotopes in a mantle-derived aluminous Ti-rich amphibole, kaersutite, were measured, and the abundance pattern indicated by the results is similar to the 'planetary' rare gas pattern of carbonaceous chondrites. The He-3/He-4 ratio of (4.9 + or - 0.6) times 10 to the -5th power is anomalously high. Ne-21 is enriched relative to the abundance of the other two neon isotopes in the atmosphere, while the heavy isotopes of Kr and the Xe isotopes are within error of the atmospheric values. The analytical procedure is described. It is concluded that part of the primordial rare gases of the earth are still present in some parts of the upper mantle and that these gases retain a faithful record of the 'planetary' primordial rare gas elemental signature.
The predicted anomalous tail of periodic comet d'Arrest was photographed and photometrically studied. The derived particle-size distribution function varies inversely according to slightly higher than the 4-th power of the size. Particle dimensions span a few orders of magnitude, the mean size being in the general range of 0.01 to 0.1 cm depending on the assumed bulk density. The determination of the amount of the ejected dust is complicated by large uncertainties in the particle albedo. The product of the particle albedo and of the production rate of meteoroids that remain gravitationally bound to the solar system is found to be about 3000 g/s at the time of maximum activity and some 200 g/s when averaged over the comet's revolution period. The contribution of the comet to the interplanetary dust cloud is insignificant, unless the albedo of the debris from the comet is as low as 0.1 percent.
The rate constant for the reaction Br + O3 yields BrO + O2 has been measured from 200 to 360 K by the technique of flash photolysis coupled to time resolved detection of bromine atoms by resonance fluorescence (FP-RF). Br atoms were produced by the flash photolysis of CH3Br at a wavelength of 165 nm. O3 concentration was monitored continuously under reaction conditions by absorption at 253.7 nm. At each of five temperatures the results were independent of substantial variations in O3 concentration, total pressure (Ar), and limited variations in flash intensity (i.e., initial Br concentration). The measured rate constants obey the Arrhenius expression, k = (7.74 plus or minus 0.50) x 10 to the -12th exp(-603 plus or minus 16/T) cu cm/molecule/sec, where the error quoted is two standard deviations.
Photoelectric observations and recently published laboratory measurements of HD imply an upper limit on the deuterium-to-hydrogen ratio in Uranus's atmosphere of D/H less than 9.6 x 10 to the -5th power. This is much closer to values currently being proposed for Jupiter
X-rays from the compact galaxy III Zw 2 have been detected with the rotating modulation collimator on board SAS 3. The (2-10-keV) flux is (4.3 + or - 0.5) by 10 to the -11th power erg/sq cm per sec, which corresponds to a luminosity of 1.4 by 10 to the 45th power erg/s at 530 Mpc. Subsequent radio observations between 1.46 and 90 GHz were made at the NRAO Very Large Array and 36-foot (11-m) installations. The radio spectrum rises sharply toward higher frequencies and, below about 100 GHz, is indicative of a self-absorbed synchrotron spectrum from an extremely compact, rapidly evolving object.
This letter reports observations of the 51.8-micron fine-structure transition p2: 3P(2) - 3P(1) for doubly ionized oxygen. The observed line strength in the Orion Nebula is (5 + or - 3) by 10 to the -15th power W/sq cm, in good agreement with the theoretical predictions of Simpson (1975). The observations are also consistent with the predicted line position, 51.8 microns. The line lies close to an atmospheric water-vapor feature at 51.7 microns but is sufficiently distant so that corrections for this feature are straightforward. Observations of the 51.8-micron forbidden O III line are particularly important, since the previously discovered 88-micron line from the same ion also is strong. This pair of lines should therefore yield new data about densities in observed H II regions; or else, if density data already are available from radio or other observations, the lines can be used to determine the differential dust absorption between 52 and 88 microns in front of heavily obscured regions.
Concentration ratios of Al/Si and Mg/Si have been determined from the orbital X-ray data for twenty-two regions for which the concentrations of Th, K, Fe, and Mg has previously been specified from orbital gamma-ray data. The strong anticorrelation between Fe and Al seen in returned samples is confirmed for large areas of the lunar surface. The natural radioactivity of the large maria increases from east to west whereas an inverse in true for the aluminum concentration. The difficulty in determining Mg concentrations in each experiment is discussed.
A correlation between orbital chemistry (FeO, Al2O3, Mg/Al, MgO/FeO, Th) and the lunar crustal thickness is examined. The correlation suggests either lack of complete homogenization by lateral or vertical mixing, or lateral variation in the differentiation process. In addition, links between orbital chemistry and lunar sample chemistry are investigated. In regions with crustal thickness between 100 and 110 km, gabbroic anorthosites are very abundant, while in regions with crustal thickness of about 80 km anorthositic gabbros are frequent. Special attention is given to the distribution of low-potassium Fra Mauro basalt, found in high concentrations in regions with 50 to 60 km crustal thickness.
Image-processing techniques applied to orbital data have revealed an inverse correlation between lunar surface remanent magnetism and surface concentrations of Fe and Th on a scale of 250 km and greater. The effect can be understood in terms of the implantation of magnetism early in the history of the moon, coupled with the chronological sequence of highland-mare crustal differentiation. The exception seen at the Fra Mauro region suggests the presence of a source of magnetization sometime within 0.3-0.6 b.y. after formation of the moon.
A quick method is described for finding the primitive (2 to power p + 1)p-th root of unity in the Galois field GF(q squared), where q = (2 to power p) - 1 and is known as a Mersenne prime. Determination of this root is necessary to implement complex integer transforms of length (2 to power k) times p over the Galois field, with k varying between 3 and p + 1.
The precise numerical integration of Cowell's equations of satellite motion is frequently performed with an independent variable s defined by an equation of the form dt = cr to the n-th power ds, where t represents time, r the radial distance from the center of attraction, c is a constant, and n is a parameter. This has been primarily motivated by the 'uniformizing' effects of such a transformation resulting in desirable 'analytic' stepsize control for elliptical orbits. This report discusses the 'proper' choice of the parameter n defining the independent variable s for various types of orbits and perturbation models, and develops a criterion for its selection.
Samples of fines less than 1-mm and 155 1-2 mm particles from several Apollo 17 sites were analyzed for Na, Sc, Cr, Mn, Fe, Co, Ni, Hf, Ta, Th, and REE. Products of comminution and construction are present in the 1-2 mm particles, and the compositions of the rock fragments clearly indicate the general chemical characteristics of their parent rock types. The likely sources of materials for the glassy particles are considered. Glasses are enriched over their parent soils in Fe, Sc, Mn, and Cr, and are relatively enriched in light REE, so that some chemical fractionation accompanies glass-forming processes. Elements were determined by instrumental neutron activation analysis.
Absolute rate constants for the deactivation of O(1D) by CO have been measured at temperatures between 113 and 333 K. A very small temperature dependence is observed and is described by the Arrhenius expression (4.7 + or - 0.9) times 10 to the -11th power exp(126 + or 33)/RT cu cm/molecule-sec, where E is in cal/mol.