An integrated study of earth resources in the State of California based on ERTS-1 and supporting aircraft data, volume 2
There are no author-identified significant results in this report.
Colwell, R. N.↗
Engineering topics
Schubert, G.
Publications and source records attributed to Schubert, G..
Analysis of river meanders from ERTS-1 imagery
There are no author-identified significant results in this report.
Colwell, R. N.↗
Night side electromagnetic response of the moon.
The inductive response of the moon to interplanetary magnetic field fluctuations has been measured by the Apollo 12 lunar surface magnetometer. The dependence of the night side lunar response on frequency in the band from about 0.001 to 0.01 Hz is reported. It is shown that the night side response of the moon is not that of a sphere in vacuum. Instead, hydromagnetic radiation scattered from the moon is strongly confined to the interior of the cavity formed downstream from the moon in the solar wind.
Schubert, G.↗
An integrated study of earth resources in the state of California using remote sensing techniques
The University of California has been conducting an investigation which seeks to determine the usefulness of modern remote sensing techniques for studying various components of California's earth resources complex. Most of the work has concentrated on California's water resources, but with some attention being given to other earth resources as well and to the interplay between them and California's water resources.
Colwell, R. N.↗
Topology of induced lunar magnetic fields.
Using the asymmetric theory of lunar induction derived by Schubert et al. (1973), a picture of both the total and induced magnetic field line distributions in and around the moon is provided for certain orientations of the interplanetary field fluctuations. These field line pictures are compared with the distributions one would obtain using a spherically symmetric vacuum theory of lunar induction. It is found that the induced lunar field line distribution bears a marked resemblance to the structure of the solar-wind distorted geomagnetic field.
Schwartz, K.↗
Orbital mapping of the lunar magnetic field.
Examination of the lunar magnetic field as deduced from the orbital magnetometer data, with major emphasis on the general mapping of the lunar field over the orbit track of the Apollo 15 subsatellite. A detailed analysis of the data from a series of overflights of the Van de Graaff region at two different altitudes is also presented. This latter set of data makes it possible to determine the scale size of the region and the contrast between the remanent magnetization associated with the magnetic feature and its surroundings. The low altitude data from the Apollo 16 subsatellite, just prior to its impact into the lunar surface, are then examined. Data obtained while the moon was in the solar wind are used to construct a map which shows the lunar limb regions associated with the detection of limb compressions. This map is used to make qualitative inferences concerning the lunar remanent field in regions not covered by the contour maps.
Sharp, L. R.↗
Induced magnetosphere of the moon. I - Theory.
An analytic solution for the magnetic field in the space defined by a spherical moon and its downstream cylindrical cavity formed by the solar wind is derived for interplanetary magnetic fields both parallel and perpendicular to the cavity axis. By superposition, the solution is obtained for arbitrary orientations of the interplanetary field. The theory is quasi-static and is formulated in terms of a scalar magnetic potential. Thus, the moon model consists of a core of arbitrary size and infinite electrical conductivity surrounded by a nonconducting shell; the cavity volume is also assumed to be nonconducting. The variation of the magnetic field on the lunar surface (both sunlit and dark hemispheres) and on the cavity boundary is presented for various values of core radius.
Schubert, G.↗
Apollo 15 and 16 subsatellite magnetometer measurements of the lunar magnetic field.
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Russell, C. T.↗
Evidence for convection in planetary interiors from first-order topography.
Center of mass/center of figure offsets are known for the earth, moon, Mars and Venus. Such an offset requires a density distribution asymmetric about the center of mass. Observational evidence indicates that the terrestrial, lunar and Martian offsets result from crusts of variable thickness rather than lateral density inhomogeneities and that the thickness variations are more likely caused by internal convection than impact.
Lingenfelter, R. E.↗
Martian centre of mass - Centre of figure offset.
A Fourier analysis of Martian radar topographic data is carried out to determine the magnitude and direction of the center-of-mass/center-of-figure offset of Mars. A value of about 1 km is obtained for the figure offset with respect to the center of mass in the general direction of Tharsis. It is noted that figure offsets of comparable magnitudes exist in the earth and the moon.
Schubert, G.↗
Topology of induced lunar magnetic fields
Using the asymmetric theory of lunar induction the total and induced magnetic field line structure within the Moon and the diamagnetic cavity were obtained. Total field distributions are shown for orientations of the oscillating interplanetary field parallel, perpendicular and at 45 deg to the cavity axis. Induced field lines are shown only for the orientations of the interplanetary field parallel and orthogonal to the cavity axis. When compared with the field lines derived using the long wavelength limit of spherically symmetric vacuum induction theory, the configurations obtained using the asymmetric theory exhibit significant distortion. For all orientations of the interplanetary field, the field lines are strongly compressed on the sunlit hemisphere because of the confining solar wind pressure at the lunar surface and the exclusion of the field by the lunar core.
Schwartz, K.↗
The induced magnetosphere of the moon. 1: Theory
An analytic solution for the magnetic field in the space defined by a spherical moon and its downstream cylindrical cavity formed by the solar wind is derived for interplanetary magnetic fields both parallel and perpendicular to the cavity axis. By superposition, the solution is obtained for arbitrary orientations of the interplanetary field. The theory is quasi-static and is formulated in terms of a scalar magnetic potential. Thus the moon model consists of a core of arbitrary size and infinite electrical conductivity surrounded by a nonconducting shell; the cavity volume is assumed to be nonconducting. The variation of the magnetic field on the lunar surface, both on the sunlit and on the dark side hemispheres, and on the cavity boundary is presented for various values of core radius. The solution yields the distribution of currents on the lunar sunlit surface and the surface of the cavity. Theoretical transfer functions are presented and their variations with position on the lunar surface and with core size are discussed.
Schubert, G.↗
Surface and orbital magnetic results from Apollo 15.
Orbital and surface measurements reveal that magnetization is a general property of the lunar surface, but show no evidence for a presently existing planetary magnetic field similar to that of the earth. The surface magnetic field is irregular with a scale size of the order of 10 km and weak in comparison with that at the surface of the earth. Fields of up to 300 gammas have been measured on the surface of the moon. Orbital data show the field is stronger and more irregular on the far side than on the near side of the moon. When the moon is in the solar wind, a plasma void occurs behind the moon, due to the absorption of the solar wind by the surface of the moon. The field strength in the plasma void is larger than that in the solar wind owing to diamagnetism.
Russell, C. T.↗
Apollo 17 laser altimeter
The performance and operation of the Apollo 17 laser altimeter after several modifications are discussed. Functions of the instrument include precise altitude measurement of the CSM above the lunar surface, and measurement of broad scale topographic relief around the entire circumference of the moon.
Wollenhaupt, W. R.↗
Lunar topography from Apollo 15 and 16 laser altimetry
In the orbital plane of Apollo 15 the mean lunar radius is 1737.3 km, the mean altitude of terrae above maria is about 3 km, and the center-of-figure is displaced from the center-of-mass by about 2 km away from longitude 25 E. The Apollo 16 laser altimeter obtained a total of about 7.5 revolutions of partially overlapping data. The principal difference in results from Apollo 16 is the absence of any great far-side basin similar to the 1400-km wide feature found by Apollo 15, 1200 km to the south. This absence of a far-side depression in the Apollo 16 orbital plane largely accounts for a greater mean radius: 1738.1 km; a greater mean altitude of terrae above maria: about 4 km; and a greater offset of centers: about 3 km, also away from 25 E. In the Apollo 16, as well as Apollo 15, data the far-side terrae are much 'rougher' than the near-side terrae. Mare surfaces are generally smooth to within plus or minus 150 m, and have slopes of 1:500 to 1:2000 persisting over distances as great as 500 km.
Kaula, W. M.↗
Subsatellite measurements of the lunar magnetic field
The Apollo 15 subsatellite magnetometer data have been used to map the lunar magnetic field over a narrow band of the lunar surface. Within this band the magnetic field is generally stronger and more variable over the farside highlands than the nearside maria. The correspondence between the strong variable lunar field regions and the source regions for limb compressions suggests that limb compressions arise as the result of the deflection of the solar wind just upstream of the terminator by the lunar magnetic field. Using this apparent relationship between field strength and limb compression source regions, it is deduced that the field strength in the northern farside highlands is not as strong as in the southern hemisphere at similar longitudes. Simultaneous measurements of the interplanetary magnetic field obtained by Explorer 35 and the Apollo 15 subsatellite above the dayside hemisphere are essentially identical. Thus, both instruments are measuring the undisturbed interplanetary field.
Russell, C. T.↗
Lunar electromagnetic scattering. II - Magnetic fields and transfer functions for parallel propagation
Magnetic field and transfer function amplitudes, resulting from a transverse electromagnetic wave in the interplanetary medium scattering from the moon and its diamagnetic cavity, are presented. Calculations are made using an asymmetric scattering theory for a spherical two-layer model of the lunar electrical conductivity profile and a nonconducting cylindrical model of the downstream lunar plasma void. Both the field and transfer function magnitudes are calculated as functions of position on the surface of the moon for frequencies relevant to the observations of the lunar surface and orbiting magnetometers. The amplitudes of the magnetic field components on the cavity boundary are also computed as functions of frequency and distance downstream from the lunar limb. Comparisons of the results are made with those of (1) spherically symmetric descriptions of lunar electromagnetic scattering, (2) the quasi-static approximation to asymmetric scattering theory, and (3) observations of the scattering phenomenon by lunar surface and orbiting magnetometers.
Schubert, G.↗
Remote sensing of stream flow rates - Correlation of meander and discharge spectra
Results of a study of river meander patterns and discharges, in which attempt was made to correlate the discharge spectrum of a river with the river meander power spectrum determined from aerial and satellite imagery. Some significant characteristics of both the discharge and the meander spectra have been discovered. Discharge frequency spectra based on long-term records of daily streamflow are found to have an inverse power-law dependence on discharge. This is shown to reflect the short-term decay of individual floods which are found to have an inverse power-law dependence on time. Meander power spectra for a number of river reaches, digitized from aerial photography, also show significant structure, the power spectral density having an inverse power-law dependence on wave number over one or more portions of the spectrum with breaks in the spectra at characteristic wave numbers. A number of examples of typical discharge and meander spectra are shown.
Lingenfelter, R. E.↗