Radar and photoelectric observations of asteroid 2100 Ra-Shalom     

Steven J. Ostro  Alan W. Harris  Donald B. Campbell  Irwin I. Shapiro  James W. Young 《Icarus》1984,60(2):391-403

Results of 13-cm-wavelength radar observations and V-filter photoelectric observations of Ra- Shalom during its 1981 Aug–Sep apparition are reported. The radar data yid detections of echoes in the same sense of circular polarization as transmitted (i.e., the SC sense) as well as in the opposite (OC) sense. The estimate of the ratio of SC to OC echo power, μ_c = 0.14 ± 0.02, indicates that most, but certainly not all, of the backscattering is due to single reflections from surface elements that are fairly smooth at decimeter scales. The value obtained for the OC radar cross section on Aug 26 (1.2 ± 0.3 km²) is about three times larger than those obtained on Aug 23, 24, and 25. The echo bandwidth appears to be within about 1.5 Hz of 5.0 Hz on each date. The photoelectric data suggest a value, P_syn = 19.79 hr, for the synodic rotation period, and yield a composite lightcurve with two pairs of extrema. Combining this value for P_syn with a firm lower bound (4 Hz) on the maximum echo bandwidth yields a lower bound of 1.4 km on the maximum distance between Ra-Shalom's spin axis and any point on its surface.  相似文献   

On the relative importance of the driving forces of plate motion   总被引：4，自引：0，他引：4  

George Backus  Jeffrey Park  David Garbasz 《Geophysical Journal International》1981,67(2):415-435

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A magnitude-frequency relation for the lognormal distribution of earthquake magnitude     

George Purcaur  Dan Zorilescu 《Pure and Applied Geophysics》1971,87(1):43-53

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Verification of a parabolic equation for propagation of weakly-nonlinear waves     

James T. Kirby  Robert A. Dalrymple 《Coastal Engineering》1984,8(3):219-232

Verification tests of linear wave propagation models for cases of waves propagating through a refractive focus typically overpredict peak amplitudes in the vicinity of the focus. Using a parabolic equation model for the combined refraction-diffraction of weakly-nonlinear waves [valid for Ursell number U_r < O(1)], we show that, in a particular experiment, much of the discrepancy between laboratory measurements and linear wave model predictions can be accounted for by including the effect of nonlinearity, which is important in the region of the focus.  相似文献   

Explosive volcanic eruptions — IV. The control of magma properties and conduit geometry on eruption column behaviour     

Lionel Wilson  R. Stephen J. Sparks  George P. L. Walker 《Geophysical Journal International》1980,63(1):117-148

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Pile capacity in a softening soil     

James D. Murff 《国际地质力学数值与分析法杂志》1980,4(2):185-189

A method for determining the load–deformation response of a pile in a softening soil is presented. The results demonstrate the degree to which the flexibility of the pile can affect its ultimate capacity.  相似文献   

RESIDENTIAL PREFERENCE PATTERNS OF AFRO-AMERICAN COLLEGE STUDENTS IN THREE DIFFERENT STATES     

James H. Johnson  Stanley D. Brunn 《The Professional geographer》1980,32(1):37-42

The residential preferences of Afro-American students in three black colleges in Pennsylvania, North Carolina, and Texas are factor analyzed to determine whether major differences exist. Mapping the factor scores for the students in each college reveals that state rankings vary markedly from one region to another, black spatial preferences differ markedly from those students attending predominately white universities, and preference patterns reflect contemporary interregional black migration trends.  相似文献   

Solar XUV limb brightening observations     

George L. Withbroe 《Solar physics》1970,11(2):208-221

Limb brightening of XUV lines of the ions Ciii Niii, Niv, Oiii, Oiv, Ov and Siiv is compared with that predicted by a modified version of a coronal model developed by Dupree and Goldberg. Systematic differences between the predicted and observed limb brightening are found. These differences can be eliminated by introducing into the model the effects of spicules that extend up into the chromospheric-coronal transition region. The spicules are assumed to be opaque to radiation between 500 and 900 Å because of absorption in the hydrogen Lyman continuum.  相似文献   

The hose-pipe instability in stellar systems     

R. M. Kulsrud  James W. K. Mark  A. Caruso 《Astrophysics and Space Science》1971,14(1):52-55

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Moonquakes and lunar tectonism   总被引：1，自引：0，他引：1  

Gary Latham  Maurice Ewing  James Dorman  David Lammlein  Frank Press  Naft Toksőz  George Sutton  Fred Duennebier  Yosio Nakamura 《Earth, Moon, and Planets》1972,4(3-4):373-382

With the succesful installation of a geophysical station at Hadley Rille, on July 31, 1971, on the Apollo 15 mission, and the continued operation of stations 12 and 14 approximately 1100 km SW, the Apollo program for the first time achieved a network of seismic stations on the lunar surface. A network of at least three stations is essential for the location of natural events on the Moon. Thus, the establishment of this network was one of the most important milestones in the geophysical exploration of the Moon. The major discoveries that have resulted to date from the analysis of seismic data from this network can be summarized as follows:

1. Lunar seismic signals differ greatly from typical terrestrial seismic signals. It now appears that this can be explained almost entirely by the presence of a thin dry, heterogeneous layer which blankets the Moon to a probable depth of few km with a maximum possible depth of about 20 km. Seismic waves are highly scattered in this zone. Seismic wave propagation within the lunar interior, below the scattering zone, is highly efficient. As a result, it is probable that meteoroid impact signals are being received from the entire lunar surface.
2. The Moon possesses a crust and a mantle, at least in the region of the Apollo 12 and 14 stations. The thickness of the crust is between 55 and 70 km and may consist of two layers. The contrast in elastic properties of the rocks which comprise these major structural units is at least as great as that which exists between the crust and mantle of the earth. (See Toks?zet al., p. 490, for further discussion of seismic evidence of a lunar crust.)
3. Natural lunar events detected by the Apollo seismic network are moonquakes and meteoroid impacts. The average rate of release of seismic energy from moonquakes is far below that of the Earth. Although present data do not permit a completely unambiguous interpretation, the best solution obtainable places the most active moonquake focus at a depth of 800 km; slightly deeper than any known earthquake. These moonquakes occur in monthly cycles; triggered by lunar tides. There are at least 10 zones within which the repeating moonquakes originate.
4. In addition to the repeating moonquakes, moonquake ‘swarms’ have been discovered. During periods of swarm activity, events may occur as frequently as one event every two hours over intervals lasting several days. The source of these swarms is unknown at present. The occurrence of moonquake swarms also appears to be related to lunar tides; although, it is too soon to be certain of this point.

These findings have been discussed in eight previous papers (Lathamet al., 1969, 1970, 1971) The instrument has been described by Lathamet al. (1969) and Sutton and Latham (1964). The locations of the seismic stations are shown in Figure 1.  相似文献