Altered basaltic glass: A terrestrial analog to the soil of Mars     

Carlton C. Allen  James L. Gooding  Michael Jercinovic  Klaus Keil 《Icarus》1981,45(2):347-369

Analyses of Martian surface soil by Viking and Earth-based telescopes have been interpreted as indicating a regolith dominated by the weathering products of mafic or ultramafic rocks. Basaltic glass has previously been proposed as a more likely precursor than crystalline rock, given the low efficiency of surface weathering under present Martian conditions. On Earth large volumes of basaltic glass formed by quenching of magma by water. A similar interaction, between magma and ground ice, may have been a common occurrence on Mars. On the basis of this scenario palagonite, the alteration product of basaltic sideromelane glass, was studied as a possible analog to Martian soil. Samples from Iceland, Alaska, Antarctica, Hawaii, and the desert of New Mexico and Mexico were examined by optical and scanning electron microscopy, electron microprobe analysis, X-ray diffraction, spectrophotometry, and magnetic and thermogravimetric analysis. We suggest that palagonite is a good analog to the surface soil of Mars in chemical composition, particle size, spectral signature, and magnetic properties. Our model for the formation of fine-grained Martian surface soil begins with eruptions of basaltic magma through ground ice, forming deposits of glassy tuff. Individual glass shards are then altered by low-temperature hydrothermal systems to palagonitic material. Dehydration and aeolian abrasion strip the alteration rinds from the glass, and wind storms distribute the silt-sized palagonitic fragments in a planet-wide deposit.  相似文献   

Off disk-center potential field calculations using vector magnetograms     

P. Venkatakrishnan  G. Allen Gary 《Solar physics》1989,120(2):235-247

We investigate a potential field calculation for off disk-center vector magnetograms that uses all the three components of the measured field. There is neither any need for interpolation of grid points between the image plane and the heliographic plane nor for an extension or a truncation to a heliographic rectangle. Hence, the method provides the maximum information content from the photospheric field as well as the most consistent potential field independent of the viewing angle. The introduction of polarimetric noise produces a less tolerant extrapolation procedure than using the line-of-sight extrapolation, but the resultant standard deviation is still small enough for the practical utility of this method.National Research Council Resident Research Associate on leave from Indian Institute of Astrophysics, Bangalore 560034, India.  相似文献   

Constraints on the176Lu cosmochronometer     

J. R. De Laeter  B. J. Allen  G. C. Lowenthal  J. W. Boldeman 《Journal of Astrophysics and Astronomy》1988,9(1):7-15

In an endeavour to resolve reported discrepancies in the value of the branching ratio of¹⁷⁶Lu at astrophysical energies, a new determineation of the¹⁷⁵Lu (nγ)^176mLu capture cross section has been measured as 958 ± 58 mb. This gives a value of the branching ratio of 0.21 ±0.05. This result indicates that some reequilibration of the ground and isomeric states of¹⁷⁶Lu occurs in stellar environments undergoing s-process nucleosynthesis, and confirms that¹⁷⁶Lu is not a reliable cosmochronometer. However the very existence of¹⁷⁶Lu in the solar system implies that the ground state of¹⁷⁶Lu was not completely depopulated, and provides the possibility of using this nuclide as a sensitive thermometer for stellar processes.  相似文献   

High-Resolution Signal and Noise Field Estimation Using theL1 (Least Absolute Values) Norm     

Zala  C. Barrodale  I. Kennedy  J. 《Oceanic Engineering, IEEE Journal of》1987,12(1):253-264

In this paper a new method for obtaining a quantitative estimate of an acoustic field consisting of a set of discrete sources and background noise is described. The method is based on theL1 (least absolute values) norm solution to an underdetermined system of linear equations defining the Fourier transform of the signal series. Implementations of the method with either equality or inequality constraints are presented and discussed. The much faster and more compact equality constraint version with a provision for modeling the noise field is recommended in practice. Experience with real data has shown the necessity of correcting for an observed Gaussian decay on the covariances. A simple means of estimating this effect and taking it into account in the signal estimation procedure is discussed, and the implications of this effect in high-resolution beamforming are considered. The effectiveness and versatility of theL1 method indicate that it has a useful role in high-resolution signal estimation.  相似文献   

On the shape of the non-steady interface intersecting discontinuities in permeability     

Jacob Bear  Allen M. Shapiro 《Advances in water resources》1984,7(3):106-112

The simplifying assumption is often made, that when two fluids (whether miscible or immiscible) occupy the void space of a porous medium, they are separated by a sharp interface. Examples are the phreatic surface (between air and water) and the interface between fresh and salt water in a coastal aquifer. The orientation of such a sharp interface as it crosses a surface of discontinuity between media of different permeabilities, and as it intersects an impervious boundary, is shown to depend not only on the fluid and porous media properties, but also on the direction and rate of motion of the interface. Thus, advancing and retreating interfaces intersect boundaries of discontinuity in permeability at different angles.  相似文献   

Evaluation of river thermal regime models     

P.P. Paily  J.F. Kennedy 《Advances in water resources》1978,1(4):219-227

  相似文献   

Book review     

Allen F. Glazner  John C. Griffiths  Betty L. Gibbs 《Mathematical Geology》1988,20(6):753-761

  相似文献   

Interplanetary proton (0.61 < E p < 3.41 MeV) events observed with Pioneer 11, 1973–1986 and out to 22.4 AU     

James A. Van Allen 《Solar physics》1987,112(1):165-179

A survey of interplanetary proton (0.61 < E _p < 3.41 MeV) events is summarized in graphical and tabular form for the period April 1973–December 1986. The observations were obtained by an effectively continuous data stream from the University of Iowa instrument on the Ames Research Center/NASA spacecraft Pioneer 11 as it moved outward in the solar system from 1.0 to 22.4 AU. Two hundred and sixty-five distinct events are identified. The spectra and intensities of the protons, presumed to be originally of solar origin, are influenced dramatically by propagative and accelerative processes in the interplanetary medium.  相似文献   

Infrared studies of the lunar terrain     

David A. Allen 《Earth, Moon, and Planets》1971,2(4):435-462

This paper presents an infrared study of thermal anomalies during the lunar night. From observations of the most intense anomalies at several wavelengths it is deduced that fields of boulders are responsible for the thermal enhancement; the cooling curves of the remainder are consistent with such a model. High resolution Lunar Orbiter photographs of some of the thermal anomalies reveal boulders to be present within them in just the right numbers. The ages and distribution of thermal anomalies are discussed in the light of this model.  相似文献   

Three components of 3–4 μm absorption bands     

D. T. Wickramasinghe  D. A. Allen 《Astrophysics and Space Science》1983,97(2):369-378

We present 2–4 μm spectra of six infrared sources for which the extinction is not purely interstellar, but is dominated by circumstellar or molecular cloud dust. In all cases the absorption bands differ from the interstellar case, though a component of the interstellar absorption is often present. We also present an improved absorption spectrum for the galactic centre source IRS 7, correcting spurious features in our previous spectrum. Three independent components can be identified: (i) The interstellar component, probably of organic origin, and itself not necessarily invariant; (ii) The symmetrical water ice feature at 3.06 μm, found most commonly in molecular clouds; (iii) A component at 3.53 μm possibly identified with solid formaldehyde grains, and seen only in molecular clouds because of its weakness. Other absorption components appear to be unrelated to those in the 3–4 μm region, most notably the 10 μm absorption found in oxygen-rich giants and the interstellar medium, and presumable inorganic in nature. Our observations include the first detection of water ice absorption in a source in the ρ Oph dark cloud. Biological materials provide the best fit to the interstellar case, but do not presently account for the distinct 3.53 μm component. We stress the need for further laboratory experiments using simpler organic materials.  相似文献