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  • 1
    Online Resource
    Online Resource
    Lunar tidal acceleration from Earth satellite orbit analyses
    American Geophysical Union (AGU) ; 1981
    In:  Journal of Geophysical Research: Solid Earth Vol. 86, No. B3 ( 1981-03-10), p. 1659-1663
    Details
    In: Journal of Geophysical Research: Solid Earth, American Geophysical Union (AGU), Vol. 86, No. B3 ( 1981-03-10), p. 1659-1663
    Abstract: We present results for the M 2 and O 1 ocean tides based on the Starlette satellite orbit analyses from which the tidal acceleration of the moon is derived. The solution for M 2 is consistent with previous satellite solutions; for O 1 we find a phase lag which is approximately zero. The uncertainty is still large, but there is an indication that the tidal dissipation at the O 1 frequency is small. Using the weighted mean value of the best satellite solutions gives = −21.32 ± 1.25 arc sec/(century) 2 for the total dissipation in the earth at the M 2 frequency. In principle, comparison between derived from satellite solution and derived from numerical models gives the amount of dissipation in the solid earth, but uncertainties are still too large to give a reliable estimate of the tidal mantle Q .
    Type of Medium: Online Resource
    ISSN: 0148-0227
    URL: Article
    DOI: 10.1029/JB086iB03p01659
    Language: English
    Publisher: American Geophysical Union (AGU)
    Publication Date: 1981
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    SSG: 16,13
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  • 2
    Online Resource
    Online Resource
    Numerical experiment applicable to the latest stage of planet growth
    Elsevier BV ; 1982
    In:  Icarus Vol. 51, No. 1 ( 1982-7), p. 133-148
    Details
    In: Icarus, Elsevier BV, Vol. 51, No. 1 ( 1982-7), p. 133-148
    Type of Medium: Online Resource
    ISSN: 0019-1035
    URL: Article
    DOI: 10.1016/0019-1035(82)90033-1
    Language: English
    Publisher: Elsevier BV
    Publication Date: 1982
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  • 3
    Online Resource
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    Thermal cooling of the oceanic lithosphere: new constraints from geoid height data
    Elsevier BV ; 1984
    In:  Earth and Planetary Science Letters Vol. 70, No. 2 ( 1984-10), p. 395-406
    Details
    In: Earth and Planetary Science Letters, Elsevier BV, Vol. 70, No. 2 ( 1984-10), p. 395-406
    Type of Medium: Online Resource
    ISSN: 0012-821X
    URL: Article
    DOI: 10.1016/0012-821X(84)90023-2
    RVK:
    TE 1000
    Language: English
    Publisher: Elsevier BV
    Publication Date: 1984
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  • 4
    Online Resource
    Online Resource
    Two distinct trends for cooling of the oceanic lithosphere
    Springer Science and Business Media LLC ; 1984
    In:  Nature Vol. 310, No. 5976 ( 1984-8), p. 401-403
    Details
    In: Nature, Springer Science and Business Media LLC, Vol. 310, No. 5976 ( 1984-8), p. 401-403
    Type of Medium: Online Resource
    ISSN: 0028-0836 , 1476-4687
    URL: Article
    DOI: 10.1038/310401a0
    RVK:
    TA 1000
    RVK:
    UA 1000
    RVK:
    WA 15000
    Language: English
    Publisher: Springer Science and Business Media LLC
    Publication Date: 1984
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  • 5
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    Online Resource
    Book review
    Springer Science and Business Media LLC ; 1981
    In:  Journal of Geodesy Vol. 55, No. 2 ( 1981-6), p. II-IX
    Details
    In: Journal of Geodesy, Springer Science and Business Media LLC, Vol. 55, No. 2 ( 1981-6), p. II-IX
    Type of Medium: Online Resource
    ISSN: 0949-7714 , 1432-1394
    URL: Article
    DOI: 10.1007/BF02530842
    Language: English
    Publisher: Springer Science and Business Media LLC
    Publication Date: 1981
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  • 6
    Online Resource
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    Numerical experiment applicable to planet formation
    Cambridge University Press (CUP) ; 1984
    In:  International Astronomical Union Colloquium Vol. 75 ( 1984), p. 675-676
    Details
    In: International Astronomical Union Colloquium, Cambridge University Press (CUP), Vol. 75 ( 1984), p. 675-676
    Abstract: A three-dimensional numerical model has been developed with the goal of studying limited dynamical problems relevant to the latest stage of planet growth in the accretion theory. A small number of large protoplanets (~ moon-size) of different masses, moving around the Sun, are considered. The dynamical evolution and growth of the population is studied under mutual gravitational perturbations, accretion and collisional fragmentation processes. Gravitational encounters are treated exactly by numerical integration of the N-body problem. Outcomes of collisional fragmentation are modeled according to the results of Greenberg et al. (1978).
    Type of Medium: Online Resource
    ISSN: 0252-9211
    URL: Article
    DOI: 10.1017/S0252921100101757
    Language: English
    Publisher: Cambridge University Press (CUP)
    Publication Date: 1984
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  • 7
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    Online Resource
    Geoid heights over the Louisville Ridge (South Pacific)
    American Geophysical Union (AGU) ; 1984
    In:  Journal of Geophysical Research: Solid Earth Vol. 89, No. B13 ( 1984-12-10), p. 11171-11179
    Details
    In: Journal of Geophysical Research: Solid Earth, American Geophysical Union (AGU), Vol. 89, No. B13 ( 1984-12-10), p. 11171-11179
    Abstract: Geoid heights over the Louisville Ridge seamount chain, deduced from the Seasat satellite altimeter data, have been analyzed and interpreted. Two uncharted seamounts belonging to the chain have been detected. The elastic thickness of the oceanic lithosphere has been determined along the chain. This was done rigorously using the three‐dimensional geoid and bathymetry maps and was also computed approximately using spectral methods on geoid and bathymetry profiles. A slightly increasing elastic thickness from the southeast to the northwest, in the range 15.5–22.5 km has been estimated.
    Type of Medium: Online Resource
    ISSN: 0148-0227
    URL: Article
    DOI: 10.1029/JB089iB13p11171
    Language: English
    Publisher: American Geophysical Union (AGU)
    Publication Date: 1984
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  • 8
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    Online Resource
    Elastic thickness of the Venus lithosphere estimated from topography and gravity
    American Geophysical Union (AGU) ; 1981
    In:  Geophysical Research Letters Vol. 8, No. 10 ( 1981-10), p. 1039-1042
    Details
    In: Geophysical Research Letters, American Geophysical Union (AGU), Vol. 8, No. 10 ( 1981-10), p. 1039-1042
    Abstract: The very close correlation observed on Venus between topography and gravity on a regional scale is clearly related to the isostatic compensation of the topographic loads. Observed gravity anomalies over topographic features of moderate lateral extent, located in the equatorial region (0° to 40° N latitude and 10° W to 60° E longitude) are somewhat larger than those computed with a model of local isostatic compensation (of Airy type). They may rather be explained by a model of compensation including elastic forces within the lithosphere which contribute to support topographic loads through elastic stresses. We have applied the theory of lithospheric flexure : to explain in wavelength and in amplitude the observed gravity anomalies, a flexural rigidity of ∼ 4 × 10 28 dyne cm has been estimated for the Venus lithosphere in the rolling plains province. This value is very low compared to the oceanic terrestrial lithosphere (ranging from ∼ 10 28 dyne cm near ridge crests to ∼ 2 × 10 31 dyne cm near subduction zones). The corresponding thickness of the elastic upper layer able to maintain elastic stresses for long time duration is ∼ 7.5 km. This value may not be representative of the entire Venus lithosphere.
    Type of Medium: Online Resource
    ISSN: 0094-8276 , 1944-8007
    URL: Article
    DOI: 10.1029/GL008i010p01039
    Language: English
    Publisher: American Geophysical Union (AGU)
    Publication Date: 1981
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  • 9
    Online Resource
    Online Resource
    Thermal parameters of the oceanic lithosphere estimated from geoid height data
    American Geophysical Union (AGU) ; 1983
    In:  Journal of Geophysical Research: Solid Earth Vol. 88, No. B2 ( 1983-02-10), p. 1105-1118
    Details
    In: Journal of Geophysical Research: Solid Earth, American Geophysical Union (AGU), Vol. 88, No. B2 ( 1983-02-10), p. 1105-1118
    Abstract: Geoid height anomalies derived from SEASAT altimeter data have been analyzed across fracture zones and over ocean ridges in two limited regions of the South Pacific (Eltanin fracture zone system; East Pacific Rise) and southeast Indian Ocean. Observed geoid height‐age and geoid height derivative (with respect to age)‐age relationships have been established. Comparison with theoretical relationships computed for the plate model of lithospheric cooling permits an estimation of the thermal parameters entering into the model. Two quantities can be derived: the product ακT m (α, thermal diffusivity; κ, volume coefficient of thermal expansion; T m , bottom boundary temperature) and the thickness H of the plate. The best fitting values for the South Pacific and the southeast Indian Ocean are ακT m = 0.52×10 −3 cm 2 s −1 and H in the range 50–70 km for ages less than 30 m.y., whereas for larger ages (≥30 m.y.), geoid observations are better explained by a larger H value, in the range 70–90 km. The depth‐age relationship observed in the South Pacific region is consistent with these parameters. On the other hand, data for the northeast Pacific argue rather for a lithospheric thickness larger than 100 km. This suggests that local and regional variations exist in the thermal properties of the oceanic lithosphere.
    Type of Medium: Online Resource
    ISSN: 0148-0227
    URL: Article
    DOI: 10.1029/JB088iB02p01105
    Language: English
    Publisher: American Geophysical Union (AGU)
    Publication Date: 1983
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  • 10
    Online Resource
    Online Resource
    Meteorological effects on the seasonal variations of the rotation of Mars
    American Geophysical Union (AGU) ; 1981
    In:  Geophysical Research Letters Vol. 8, No. 3 ( 1981-03), p. 245-248
    Details
    In: Geophysical Research Letters, American Geophysical Union (AGU), Vol. 8, No. 3 ( 1981-03), p. 245-248
    Abstract: We have investigated the meteorologically induced seasonal variations in the rotation rate of Mars. As on Earth, meteorological effects are expected to produce fluctuations in the rotation of Mars but unlike on Earth, where zonal winds are the major contributors, on Mars seasonal variations are mainly the result of exchange of CO 2 between atmosphere and polar caps through a variation of the polar moment of inertia. From Viking pressure data and zonal winds models by Haberle et al. [1979] we predict an annual and a semi‐annual cycles in the relative rotation rate of Mars of amplitude ∼ 0.2 × 10 −8 and 0.1 × 10 −8 respectively. On the length of the martian day these seasonal changes are 0.17 ms and 0.09 ms respectively. Between the fall equinox and winter solstice (northern hemisphere), the maximum change in the martian l.o.d. amounts to 0.44 ms.
    Type of Medium: Online Resource
    ISSN: 0094-8276 , 1944-8007
    URL: Article
    DOI: 10.1029/GL008i003p00245
    Language: English
    Publisher: American Geophysical Union (AGU)
    Publication Date: 1981
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