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  • Other Sources  (22)
  • NASA Technical Reports  (22)
  • 1975-1979  (14)
  • 1970-1974  (8)
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  • Other Sources  (22)
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  • 1
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    Thermal history and evolution of the moon. (1973)
    In:  Other Sources
    Details
    Publication Date: 2019-06-27
    Description: In this work, theoretical lunar temperature models are computed taking into account different initial conditions to represent possible accretion models and various abundances of heat sources to correspond to different compositions. Differentiation and convection are simulated in the numerical computational scheme. Models of the thermal evolution of the moon that fit the chronology of igneous activity on the lunar surface, the stress history of the lunar lithosphere implied by the presence of mascons, and the surface concentrations of radioactive elements, involve extensive differentiation early in lunar history. This differentiation may be the result of rapid accretion and large-scale melting or of primary chemical layering during accretion. Differences in present-day temperatures for these two possibilities are significant only in the inner 1000 km of the moon and are not resolvable with presently available data.
    Keywords: SPACE SCIENCES
    Type: The Moon; 7; May-June
    Format: text
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  • 2
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    Thermal evolution of the moon. (1972)
    In:  Other Sources
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    Publication Date: 2019-06-27
    Description: The thermal history and current state of the lunar interior are investigated using constraints imposed by recent geological and physical data. Theoretical temperature models are computed taking into account different initial conditions, heat sources, differentiation and simulated convection. To account for the early formation of the lunar highlands, the time duration of magmatism and present-day temperatures estimated from lunar electrical conductivity profiles, it is necessary to restrict initial temperatures and abundances of radioactive elements. Successful models require that the outer half of the moon initially heated to melting temperatures, probably due to rapid accretion. Differentiation of radioactive heat sources toward the lunar surface occurred during the first 1.6 billion years. Temperatures in the outer 500 km are currently low, while the deep interior (radius less than 700 to 1000 km) is warmer than 1000 C, and is of primordial material.
    Keywords: SPACE SCIENCES
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  • 3
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    The relationship between crustal tectonics and internal evolution in the moon and Mercury (1977)
    In:  Other Sources
    Details
    Publication Date: 2019-06-27
    Description: The relationship between crustal tectonics and thermal evolution is discussed in terms of the moon and Mercury. Finite strain theory and depth and temperature-dependent thermal expansion are used to evaluate previous conclusions about early lunar history. Factors bringing about core differentiation in the first 0.6 b.y. of Mercurian evolution are described. The influence of concentrating radioactive heat sources located in Mercury's crust on the predicted contraction is outlined. The predicted planetary volume change is explored with regard to quantitative limits on the extent of Mercurian core solidification. Lunar and Mercurian thermal stresses involved in thermal evolution are reviewed, noting the history of surface volcanism. It is concluded that surface faulting and volcanism are closely associated with the thermal evolution of the whole planetary volume. As the planet cools or is heated, several types of tectonic and volcanic effects may be produced by thermal stress occurring in the lithosphere.
    Keywords: LUNAR AND PLANETARY EXPLORATION
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  • 4
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    Structure of the moon (1974)
    In:  Other Sources
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    Publication Date: 2019-06-27
    Description: Seismic data fron the four stations of the Apollo passive seismic network have been analyzed to obtain the velocity structure of the moon. Analysis of body wave phases from artificial impacts of known impact time and position yields a crustal section. In the Mare Cognitum region the crust is about 60 km thick and is layered. In the 20-km-thick upper layer, velocity gradients are high and microcracks may play an important role. The 40-km-thick lower layer has a nearly constant 6.8-km/sec velocity. There may be a thin high-velocity layer present beneath the crust. The determination of seismic velocities in the lunar mantle is attempted by using natural impacts and deep moonquakes. The simplest model that can be proposed for the mantle consists of a 'lithosphere' overlying an 'asthenosphere'.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Reviews of Geophysics and Space Physics; 12; Nov. 197
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  • 5
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    Mercury - Internal structure and thermal evolution (1974)
    In:  Other Sources
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    Publication Date: 2019-06-27
    Description: Mercury's thermal evolution and internal structure are modeled based on the planet's gross physical properties (which imply a high metallic iron content) and predictions for its chemistry made from the Lewis-Cameron model of condensation of the primitive solar nebula (which implies that Mercury may be composed only of those materials that condensed at temperatures near that of metallic iron condensation in the cooling nebula). Various heat sources, initial temperatures, and thermal conductivities are considered for a homogeneous model and a differentiated two-layer model. Density distributions are calculated from the mean density and estimates of the present-day temperature. The moment of inertia and the hydrostatic value of the second degree harmonic coefficient of Mercury's gravity field are found for the differentiated and undifferentiated models. These results should be useful for preliminary interpretation of the Mariner 10 measurements of Mercury's gravitational field.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Icarus; 23; Oct. 197
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  • 6
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    Density within the moon and implications for lunar composition (1974)
    In:  Other Sources
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    Publication Date: 2019-06-27
    Description: A number of simple density models for the moon are discussed. The considered models are consistent with the lunar mass and moment of inertia, the latest information on the seismic velocity of the lunar crust and mantle, and assorted estimates of temperature in the lunar interior. New material presented includes the implications for density models of recent seismic evidence for a thin, high velocity layer beneath the lunar crust and for a zone of partial melting below 1000 km depth. The consequences of a dense, iron-rich central core are also explored.
    Keywords: SPACE SCIENCES
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  • 7
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    Some aspects of core formation in Mercury (1976)
    In:  Other Sources
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    Publication Date: 2019-06-27
    Description: Some questions dealing with the nature and history of a large metallic core within Mercury are considered. These include the existence of a core, its size, whether it is fluid or solid, the timescale for core formation, the geological consequences of core formation, and whether such consequences are consistent with the surface geology. Several indirect lines of evidence are discussed which suggest the presence of a large iron-rich core. A core-formation model is examined in which core infall is accompanied by an increase of 17 km in planetary radius, an increase of 700 K in mean internal temperature, and substantial melting of the mantle. It is argued that if the core differentiated from an originally homogeneous planet, that event must have predated the oldest geological units comprising most of the planetary surface. A convective dynamo model for the source of Mercury's magnetic field is shown to conflict with cosmochemical models that do not predict a substantial radiogenic heat source in the core.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Icarus; 28; Aug. 197
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  • 8
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    Elastic lithosphere thickness on the moon from mare tectonic features - A formal inversion (1979)
    In:  Other Sources
    Details
    Publication Date: 2019-07-13
    Description: The thickness (T) of the lunar elastic lithosphere at the time (3.6 to 3.8 billion years ago) of the earliest preserved basalt flows in circular mare basins can be estimated by inverting the observed locations of extensional tectonic features in and surrounding the maria. In performing the inversion, the lithosphere is modeled as an elastic shell with a liquid interior, and the basalt load for each mare is approximated by a set of concentric cylinders. To permit solving the forward problem of placing radial limits on the positions of the rilles around a given mare, an additional parameter F, the ratio of the radial stress at the radial limits to the maximum radial stress, is introduced. T and F are chosen to give the best weighted-squares fit of the radial limits to the observations, and are used as the initial values in a linearized matrix inversion to check the resolution and estimate errors. The application of the procedure to three maria with prominent extensional features, Humorum, Orientale, and Serenitatis, gives values of T from about 40 + or - 10 to 50 + or - 10 km, and in each case the linearized matrix equation has an exact inverse.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Lunar and Planetary Science Conference; Mar 19, 1979 - Mar 23, 1979; Houston, TX
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  • 9
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    Mare volcanism and lunar crustal structure (1975)
    In:  Other Sources
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    Publication Date: 2019-07-13
    Description: It is pointed out that the concept of hydrostatic head, the height to which a fluid at a given pressure will rise in a gravitational field, can be usefully applied to magmatic liquids and to a number of problems in volcanology. For the moon, hydrostatic head arguments are an essential ingredient to explanations of mascons and of the scarcity of farside maria. In the reported investigation, simple hydrostatic concepts are extended to synthesize results from experimental petrology, lunar chronology, thermal history models, seismology, and gravity. Attention is given to a scenario for early lunar history, the density of lunar rocks and basaltic liquids, the thickness of the lunar crust, the source depth of mare basalt versus time, hydrostatic considerations with respect to the occurrence of high-titanium and low-titanium mare basalts, the structure of mascons, and the extension of the concepts of hydrostatics to the parent liquids of other basaltic rocks returned from the lunar surface.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Lunar Science Conference; Mar 17, 1975 - Mar 21, 1975; Houston, TX
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  • 10
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    Some aspects of core formation in Mercury (1975)
    In:  CASI
    Details
    Publication Date: 2019-07-13
    Description: An evaluation of existing theories on the existence of the planet's metallic core is presented. Topics considered are: (1) magnetic fields; (2) surface geology; (3) cosmochemical models.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: NASA-CR-143322 , Intern. Colloq. on Mercury; Jun 01, 1975
    Format: application/pdf
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