Издательство Wiley по журналам "Journal of Geophysical Research: Planets"
Отображаемые элементы 21-40 из 215
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(1992-07-25)Laboratory experiments allow the investigation of complex interactions between impacts and an atmosphere. Although small in scale, they can provide essential first‐order constraints on the processes affecting late‐stage ...
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(1995-03-25)We examine the effects of a dusty CO2 atmosphere on the thermal inertia and thermally derived albedo of Mars and we present a new map of thermal inertias. This new map was produced using a coupled surface atmosphere (CSA) ...
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(1995-04-25)Previous spectral analyses have given evidence of collisionally excited Jovian and (at times) Saturnian H2 Werner bands being absorbed by hydrocarbons at the shortest wavelengths along the auroral ovals, and of a longitudinal ...
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(1995-05-25)A number of planetary objects exhibit large radar reflectivity and polarization ratios, and more recently, a similar behavior has been observed over a vast portion of the Earth's surface: the percolation facies of the ...
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(1996-01-25)A determination of the mixing ratio of 14CO2 in the Martian atmosphere would provide a direct measurement of the degree of exchange of CO2 in the Martian atmosphere with CO2 in the regolith and polar caps. This is the case ...
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(1995-01-25)Recent calculations of the Martian obliquity suggest that it varies chaotically on timescales longer than about 107 years and varies between about 0 and 60°. We examine the seasonal water behavior at obliquities between ...
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(1993-05-25)
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(1995-04-25)Previous spectral analyses have given evidence of collisionally excited Jovian and (at times) Saturnian H2 Werner bands being absorbed by hydrocarbons at the shortest wavelengths along the auroral ovals, and of a longitudinal ...
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(1993-05-25)
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Comparisons of peak ionosphere pressures at Mars and Venus with incident solar wind dynamic Pressure(1992-01-25)Previous calculations of the potential for pressure balance between the solar wind and the ionospheres of the weakly magnetized planets, Mars and Venus, indicated that the maximum or peak ionospheric thermal pressure is ...
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(1996-01-25)In order to quantitatively assess the composition of the lunar surface from reflectance spectroscopy, it is necessary to be able to differentiate between the optical effects due to composition and those due to exposure to ...
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(1991-08-25)Finite element simulations of axisymmetric spherical shell compressible convection were carried out to investigate the effect of various surface boundary conditions in a Venusian mantle. We employed a thermal expansivity ...
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(1993-09-25)Contractional features on Mars were identified on the basis of photogeologic evidence of crustal shortening and comparison with terrestrial and planetary analogs. Three classes of structures, wrinkle ridges, lobate scarps ...
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(1996-01-25)A numerical model of the thermal evolution of Mars was developed, solving simultaneously the equations for energy conservation and hydrostatic equilibrium throughout the planet, and using an equation of state that includes ...
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(1994-03-25)Similar to the coldest terrestrial periglacial regions like Yakutia (Siberia), the planet Mars exhibits wide outflow channels. This analogy and the presence of permanent ground ice suggest that thermal erosion have existed ...
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Control of VLF burst activity in the nightside ionosphere of Venus by the magnetic field orientation(1992-07-25)In order to determine whether VLF bursts observed in the nightside ionosphere on Venus are better interpreted as whistler mode waves or ion acoustic waves we have performed both case studies and statistical studies of the ...
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(1991-11-25)Coronae on Venus are circular to elongate structures with maximum widths of 150–1000 km characterized by annuli of concentric ridges surrounding complex interiors. The features have raised topography relative to the ...
Отображаемые элементы 21-40 из 215