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  • Articles  (3,048)
  • Springer Nature  (2,673)
  • American Meteorological Society (AMS)
  • Annual Reviews
  • Emerald
  • 2005-2009  (2,845)
  • 1980-1984  (203)
  • Geosciences  (3,048)
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  • Articles  (3,048)
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Year
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  • 1
    Electronic Resource
    Electronic Resource
    Palo Alto, Calif. : Annual Reviews
    Annual Review of Earth and Planetary Sciences 10 (1982), S. 235-256 
    ISSN: 0084-6597
    Source: Annual Reviews Electronic Back Volume Collection 1932-2001ff
    Topics: Geosciences , Physics
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  • 2
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    Palo Alto, Calif. : Annual Reviews
    Annual Review of Earth and Planetary Sciences 33 (2005), S. 605-643 
    ISSN: 0084-6597
    Source: Annual Reviews Electronic Back Volume Collection 1932-2001ff
    Topics: Geosciences , Physics
    Notes: Various forms of atmospheric moist convection are reviewed through a consideration of three prevalent regimes: stratocumulus; trade-wind; and deep, precipitating, maritime convection. These regimes are chosen because they are structural components of the general circulation of the atmosphere and because they highlight distinguishing features of this polymorphous phenomenon. In particular, the ways in which varied forms of moist convection communicate with remote parts of the flow through mechanisms other than the rearrangement of fluid parcels are emphasized. These include radiative, gravity wave, and/or microphysical (precipitation) processes. For each regime, basic aspects of its phenomenology are presented along with theoretical frameworks that have arisen to help rationalize the phenomenology. Recent developments suggest that the increased capacity for numerical simulation and increasingly refined remote sensing capabilities bodes well for major advances in the coming years.
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  • 3
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    Palo Alto, Calif. : Annual Reviews
    Annual Review of Earth and Planetary Sciences 33 (2005), S. 461-491 
    ISSN: 0084-6597
    Source: Annual Reviews Electronic Back Volume Collection 1932-2001ff
    Topics: Geosciences , Physics
    Notes: Recent developments in volcanic seismology include new techniques to improve earthquake locations that have changed clouds of earthquakes to lines (faults) for high-frequency events and small volumes for low-frequency (LF) events. Spatial mapping of the b-value shows regions of normal b and high b anomalies at depths of 3-4 and 7-10 km. Increases in b precede some eruptions. LF events and very-long-period (VLP) events have been recorded at many volcanoes, and models are becoming increasingly sophisticated. Deep long-period (LP) events are fairly common, but may represent several processes. Acoustic sensors have greatly improved the study of volcanic explosions. Volcanic tremor is stronger for fissure eruptions, phreatic eruptions, and higher gas contents. Path and site effects can be extreme at volcanoes. Seismicity at volcanoes is triggered by large earthquakes, although mechanisms are still uncertain. A number of volcanoes have significant deformation with very little seismicity. Tomography has benefited from improved techniques and better instrumental arrays.
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  • 4
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    Palo Alto, Calif. : Annual Reviews
    Annual Review of Earth and Planetary Sciences 33 (2005), S. 571-604 
    ISSN: 0084-6597
    Source: Annual Reviews Electronic Back Volume Collection 1932-2001ff
    Topics: Geosciences , Physics
    Notes: Contrary to Earth, the interior of terrestrial planets is poorly known. This is mainly related to the lack of seismic data and of planetary seismic networks on these planets. So far, despite several attempts, only the Apollo Seismic Network has returned seismic information from the Moon. But even in this case, very few seismic signals were recorded after a propagation path through the deep interior and core owing to a hemispheric distribution of the stations on the near side and to a probably strongly attenuating lower mantle. This review presents the main results achieved by the analysis of the Apollo seismic data and the associated constraints on the internal structure of the Moon. It then presents the current knowledge on the Martian interior, the seismic activity of the planet, and possible source of seismic noise. This information can be used for preparing future Martian seismic network missions. A short review on existing space-qualified instruments and on possible seismic missions toward other telluric bodies, such as Venus, the giant planets' satellites, or small bodies, is then given.
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  • 5
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    Palo Alto, Calif. : Annual Reviews
    Annual Review of Earth and Planetary Sciences 33 (2005), S. 493-530 
    ISSN: 0084-6597
    Source: Annual Reviews Electronic Back Volume Collection 1932-2001ff
    Topics: Geosciences , Physics
    Notes: We know that giant planets played a crucial role in the making of our Solar System. The discovery of giant planets orbiting other stars is a formidable opportunity to learn more about these objects, what their composition is, how various processes influence their structure and evolution, and most importantly how they form. Jupiter, Saturn, Uranus, and Neptune can be studied in detail, mostly from close spacecraft flybys. We can infer that they are all enriched in heavy elements compared to the Sun, with the relative global enrichments increasing with distance to the Sun. We can also infer that they possess dense cores of varied masses. The intercomparison of presently characterized extrasolar giant planets shows that they are also mainly made of hydrogen and helium, but that they either have significantly different amounts of heavy elements, have had different orbital evolutions, or both. Hence, many questions remain and need to be answered to make significant progress on the origins of planets.
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  • 6
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    Palo Alto, Calif. : Annual Reviews
    Annual Review of Earth and Planetary Sciences 33 (2005), S. 645-671 
    ISSN: 0084-6597
    Source: Annual Reviews Electronic Back Volume Collection 1932-2001ff
    Topics: Geosciences , Physics
    Notes: The influence of surface orography on patterns of precipitation gives rise to some of the most pronounced climate gradients on Earth, and plays a fundamental role in the interaction between the atmosphere and the rest of the Earth System on a wide variety of time scales. The physical mechanisms involved comprise a rich set of interactions encompassing fluid dynamics, thermodynamics, and micron-scale cloud processes, as well as being dependent on the larger-scale patterns of the atmospheric general circulation. Investigations into orographic precipitation have pursued three parallel tracks of inquiry: observations, theory, and modeling. Significant advances have been made in each over the last few decades, and these are summarized and synthesized here. While many aspects of the basic mechanisms responsible for orographic precipitation have been understood, important issues remain unresolved. The sheer number of contributing processes, together with their convoluted interactions, make the quantitative prediction of precipitation in complex terrain a very hard task. However, while prediction of precipitation amounts for any given event may be difficult, various lines of evidence suggest that the patterns of orgraphic precipitation, even on scales of a few kilometers, are much more robust.
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  • 7
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    Palo Alto, Calif. : Annual Reviews
    Annual Review of Earth and Planetary Sciences 9 (1981), S. 59-80 
    ISSN: 0084-6597
    Source: Annual Reviews Electronic Back Volume Collection 1932-2001ff
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  • 8
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    Palo Alto, Calif. : Annual Reviews
    Annual Review of Earth and Planetary Sciences 33 (2005), S. 133-161 
    ISSN: 0084-6597
    Source: Annual Reviews Electronic Back Volume Collection 1932-2001ff
    Topics: Geosciences , Physics
    Notes: The bulk of the Đ♯50-km-thick Martian crust formed at Đ♯4.5 Gyr B.P., perhaps from a magma ocean. This crust is probably a basaltic andesite or andesite and is enriched in incompatible and heat-producing elements. Later additions of denser basalt to the crust were volumetrically minor, but resurfaced significant portions of the Northern hemisphere. A significant fraction of the total thickness of the crust was magnetized prior to 4 Gyr B.P., with the magnetization later selectively removed by large impacts. Early large impacts also modified the hemispheric contrast in crustal thickness (the dichotomy), which was possibly caused by long-wavelength mantle convection. Subsequent Noachian modification of the crust included further impacts, significant fluvial erosion, and volcanism associated with the formation of the Tharsis rise. Remaining outstanding questions include the origin of the dichotomy and the nature of the magnetic anomalies.
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  • 9
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    Palo Alto, Calif. : Annual Reviews
    Annual Review of Earth and Planetary Sciences 33 (2005), S. 247-276 
    ISSN: 0084-6597
    Source: Annual Reviews Electronic Back Volume Collection 1932-2001ff
    Topics: Geosciences , Physics
    Notes: Processes operating beneath glaciers can have a greater influence on flow dynamics than those operating within them. The variety and complexity of these processes, which involve interactions among ice, water, and geological solids, resist efforts to establish simple truths and can lead to surprising outcomes. Thermal conditions at the ice-bed interface (melting or nonmelting) and the mechanical properties of the glacier substrate (soft or hard) determine which processes can be activated. The warm-soft case supports the greatest variety of processes and is the most important for fast-flow dynamics and for the mobilization of subglacial sediment. Process interactions can lead to oscillations and spatio-temporal switching behavior in glaciers and ice sheets as well as to the generation of subglacial landforms.
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  • 10
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    Palo Alto, Calif. : Annual Reviews
    Annual Review of Earth and Planetary Sciences 33 (2005), S. 421-442 
    ISSN: 0084-6597
    Source: Annual Reviews Electronic Back Volume Collection 1932-2001ff
    Topics: Geosciences , Physics
    Notes: The Ediacara biota (575Đ??542 Ma) marks the first appearance of large, architecturally complex organisms in Earth history. Present evidence suggests that the Ediacara biota included a mixture of stem- and crown-group radial animals, stem-group bilaterian animals, "failed experiments" in animal evolution, and perhaps representatives of other eukaryotic kingdoms. These soft-bodied organisms were preserved under (or rarely within) event beds of sand or volcanic ash, and four distinct preservational styles (Flinders-, Fermeuse-, Conception-, and Nama-style) profoundly affected the types of organisms and features that could be preserved. Even the earliest Ediacaran communities (575Đ??565 Ma) show vertical and lateral niche subdivision of the sessile, benthic, filter-feeding organisms, which is strikingly like that of Phanerozoic and modern communities. Later biological and ecological innovations include mobility (〉555 Ma), calcification (550 Ma), and predation (〈549 Ma). The Ediacara biota abruptly disappeared 542 million years ago, probably as a consequence of mass extinction andor biological interactions with the rapidly evolving animals of the Cambrian explosion.
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  • 11
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    Palo Alto, Calif. : Annual Reviews
    Annual Review of Earth and Planetary Sciences 33 (2005), S. 571-604 
    ISSN: 0084-6597
    Source: Annual Reviews Electronic Back Volume Collection 1932-2001ff
    Topics: Geosciences , Physics
    Notes: Contrary to Earth, the interior of terrestrial planets is poorly known. This is mainly related to the lack of seismic data and of planetary seismic networks on these planets. So far, despite several attempts, only the Apollo Seismic Network has returned seismic information from the Moon. But even in this case, very few seismic signals were recorded after a propagation path through the deep interior and core owing to a hemispheric distribution of the stations on the near side and to a probably strongly attenuating lower mantle. This review presents the main results achieved by the analysis of the Apollo seismic data and the associated constraints on the internal structure of the Moon. It then presents the current knowledge on the Martian interior, the seismic activity of the planet, and possible source of seismic noise. This information can be used for preparing future Martian seismic network missions. A short review on existing space-qualified instruments and on possible seismic missions toward other telluric bodies, such as Venus, the giant planets' satellites, or small bodies, is then given.
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  • 12
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    Palo Alto, Calif. : Annual Reviews
    Annual Review of Earth and Planetary Sciences 8 (1980), S. 65-93 
    ISSN: 0084-6597
    Source: Annual Reviews Electronic Back Volume Collection 1932-2001ff
    Topics: Geosciences , Physics
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  • 13
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    Palo Alto, Calif. : Annual Reviews
    Annual Review of Earth and Planetary Sciences 8 (1980), S. 169-190 
    ISSN: 0084-6597
    Source: Annual Reviews Electronic Back Volume Collection 1932-2001ff
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  • 14
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    Palo Alto, Calif. : Annual Reviews
    Annual Review of Earth and Planetary Sciences 8 (1980), S. 205-230 
    ISSN: 0084-6597
    Source: Annual Reviews Electronic Back Volume Collection 1932-2001ff
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  • 15
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    Palo Alto, Calif. : Annual Reviews
    Annual Review of Earth and Planetary Sciences 11 (1983), S. 415-457 
    ISSN: 0084-6597
    Source: Annual Reviews Electronic Back Volume Collection 1932-2001ff
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  • 16
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    Palo Alto, Calif. : Annual Reviews
    Annual Review of Earth and Planetary Sciences 12 (1984), S. 133-153 
    ISSN: 0084-6597
    Source: Annual Reviews Electronic Back Volume Collection 1932-2001ff
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  • 17
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    Palo Alto, Calif. : Annual Reviews
    Annual Review of Earth and Planetary Sciences 12 (1984), S. 205-243 
    ISSN: 0084-6597
    Source: Annual Reviews Electronic Back Volume Collection 1932-2001ff
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  • 18
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    Palo Alto, Calif. : Annual Reviews
    Annual Review of Earth and Planetary Sciences 12 (1984), S. 337-357 
    ISSN: 0084-6597
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  • 19
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    Palo Alto, Calif. : Annual Reviews
    Annual Review of Earth and Planetary Sciences 12 (1984), S. 445-488 
    ISSN: 0084-6597
    Source: Annual Reviews Electronic Back Volume Collection 1932-2001ff
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  • 20
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    Palo Alto, Calif. : Annual Reviews
    Annual Review of Earth and Planetary Sciences 10 (1982), S. 327-353 
    ISSN: 0084-6597
    Source: Annual Reviews Electronic Back Volume Collection 1932-2001ff
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  • 21
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    Palo Alto, Calif. : Annual Reviews
    Annual Review of Earth and Planetary Sciences 10 (1982), S. 409-440 
    ISSN: 0084-6597
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  • 22
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    Palo Alto, Calif. : Annual Reviews
    Annual Review of Earth and Planetary Sciences 11 (1983), S. 1-10 
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  • 23
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    Palo Alto, Calif. : Annual Reviews
    Annual Review of Earth and Planetary Sciences 11 (1983), S. 99-132 
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  • 24
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    Palo Alto, Calif. : Annual Reviews
    Annual Review of Earth and Planetary Sciences 11 (1983), S. 215-240 
    ISSN: 0084-6597
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  • 25
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    Palo Alto, Calif. : Annual Reviews
    Annual Review of Earth and Planetary Sciences 11 (1983), S. 329-358 
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  • 26
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    Palo Alto, Calif. : Annual Reviews
    Annual Review of Earth and Planetary Sciences 11 (1983), S. 461-494 
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  • 27
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    Palo Alto, Calif. : Annual Reviews
    Annual Review of Earth and Planetary Sciences 12 (1984), S. 61-82 
    ISSN: 0084-6597
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  • 28
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    Palo Alto, Calif. : Annual Reviews
    Annual Review of Earth and Planetary Sciences 12 (1984), S. 179-204 
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  • 29
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    Palo Alto, Calif. : Annual Reviews
    Annual Review of Earth and Planetary Sciences 12 (1984), S. 411-443 
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  • 30
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    Annual Review of Earth and Planetary Sciences 33 (2005), S. 247-276 
    ISSN: 0084-6597
    Source: Annual Reviews Electronic Back Volume Collection 1932-2001ff
    Topics: Geosciences , Physics
    Notes: Processes operating beneath glaciers can have a greater influence on flow dynamics than those operating within them. The variety and complexity of these processes, which involve interactions among ice, water, and geological solids, resist efforts to establish simple truths and can lead to surprising outcomes. Thermal conditions at the ice-bed interface (melting or nonmelting) and the mechanical properties of the glacier substrate (soft or hard) determine which processes can be activated. The warm-soft case supports the greatest variety of processes and is the most important for fast-flow dynamics and for the mobilization of subglacial sediment. Process interactions can lead to oscillations and spatio-temporal switching behavior in glaciers and ice sheets as well as to the generation of subglacial landforms.
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  • 31
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    Annual Review of Earth and Planetary Sciences 33 (2005), S. 301-333 
    ISSN: 0084-6597
    Source: Annual Reviews Electronic Back Volume Collection 1932-2001ff
    Topics: Geosciences , Physics
    Notes: Microbes are recognized as important components of the Earth system, playing key roles in controlling the composition of the atmosphere and surface waters, forming the basis of the marine food web, and the cycling of chemicals in the ocean. A revolution in microbial ecology has occurred in the past 15Đ??20 years with the advent of rapid methods for discovering and sequencing the genes of uncultivated microbes from natural environments. Initially based on sequences from the 16S rRNA gene, this revolution made it possible to identify microorganisms without first cultivating them, to discover and characterize the immense previously unsuspected diversity of the microbial world, and to reconstruct the evolutionary relationships among microbes. Subsequent focus on functional genes, those that encode enzymes that catalyze biogeochemical transformations, and current work on larger DNA fragments and entire genomes make it possible to link microbial diversity to ecosystem function. These approaches have yielded insights into the regulation of microbial activity and proof of the microbial role in biogeochemical processes previously unknown. Questions raised by the molecular revolution, which are now the focus of microbial ecology research, include the significance of microbial diversity and redundancy to biogeochemical processes and ecosystem function.
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  • 32
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    Annual Review of Earth and Planetary Sciences 33 (2005), S. 1-36 
    ISSN: 0084-6597
    Source: Annual Reviews Electronic Back Volume Collection 1932-2001ff
    Topics: Geosciences , Physics
    Notes: This paper reviews the Precambrian history of atmospheric oxygen, beginning with a brief discussion of the possible nature and magnitude of life before the evolution of oxygenic photosynthesis. This is followed by a summary of the various lines of evidence constraining oxygen levels through time, resulting in a suggested history of atmospheric oxygen concentrations. Also reviewed are the various processes regulating oxygen concentrations, and several models of Precambrian oxygen evolution are presented. A sparse geologic record, combined with uncertainties as to its interpretation, yields only a fragmentary and imprecise reading of atmospheric oxygen evolution. Nevertheless, oxygen levels have increased through time, but not monotonically, with major and fascinating swings to both lower and higher levels.
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  • 33
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    Palo Alto, Calif. : Annual Reviews
    Annual Review of Earth and Planetary Sciences 8 (1980), S. 489-525 
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  • 34
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    Annual Review of Earth and Planetary Sciences 8 (1980), S. 407-424 
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  • 35
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    Palo Alto, Calif. : Annual Reviews
    Annual Review of Earth and Planetary Sciences 8 (1980), S. 527-558 
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  • 36
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    Annual Review of Earth and Planetary Sciences 9 (1981), S. 449-484 
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  • 37
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    Annual Review of Earth and Planetary Sciences 33 (2005), S. 195-214 
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    Source: Annual Reviews Electronic Back Volume Collection 1932-2001ff
    Topics: Geosciences , Physics
    Notes: Real-time seismology refers to a practice in which seismic data are collected and analyzed quickly after a significant seismic event, so that the results can be effectively used for postearthquake emergency response and early warning. As the technology of seismic instrumentation, telemetry, computers, and data storage facility advances, the real-time seismology for rapid postearthquake notification is essentially established. Research for early warning is still underway. Two approaches are possible: (a) regional warning and (b) on-site (or site-specific) warning. In (a), the traditional seismological method is used to locate an earthquake, determine the magnitude, and estimate the ground motion at other sites. In (b), the beginning of the ground motion (mainly P wave) observed at a site is used to predict the ensuing ground motion at the same site. An effective approach to on-site warning is discussed in light of earthquake rupture physics.
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  • 38
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    Annual Review of Earth and Planetary Sciences 33 (2005), S. 369-393 
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    Notes: Stable cratons and stable continental platforms are salient features of the Earth. Mantle xenoliths provide detailed data on deep structure. Cratonal lithosphere is about 200 km thick. It formed in the Archean by processes analogous to modern tectonics and has been stable beneath the larger cratons since that time. Its high viscosity, high yield strength, and chemical buoyancy protected it from being entrained by underlying stagnant lid convection and by subduction. Chemically buoyant mantle does not underlie platforms. Platform lithosphere has gradually thickened with time as convection waned as the Earth's interior cooled. The thermal contraction associated with this thickening causes platforms to subside relative to cratons. At present, the thickness of platform lithosphere is comparable to that of cratonal lithosphere.
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    Annual Review of Earth and Planetary Sciences 33 (2005), S. 335-367 
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    Notes: Earthquake triggering is the process by which stress changes associated with an earthquake can induce or retard seismic activity in the surrounding region or trigger other earthquakes at great distances. Calculations of static Coulomb stress changes associated with earthquake slip have proven to be a powerful tool in explaining many seismic observations, including aftershock distributions, earthquake sequences, and the quiescence of broad, normally active regions following large earthquakes. Delayed earthquake triggering, which can range from seconds to decades, can be explained by a variety of time-dependent stress transfer mechanisms, such as viscous relaxation, poroelastic rebound, or afterslip, or by reductions in fault friction, such as predicted by rate and state constitutive relations. Rapid remote triggering of earthquakes at great distances (from several fault lengths to 1000s of km) is best explained by the passage of transient (dynamic) seismic waves, which either immediately induce Coulomb-type failure or initiate a secondary mechanism that induces delayed triggering. The passage of seismic waves may also play a significant role in the triggering of near-field earthquakes.
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    Annual Review of Earth and Planetary Sciences 33 (2005), S. 443-459 
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    Notes: The mathematical modeling of landform evolution consists of two components: the processes represented (i.e., considered dominant) in the model and the (typically computer) model representation of these processes. This review discusses the current debates surrounding processes represented in landform evolution. The potential impact on both evolving landforms and computer model structure is discussed. Issues specifically discussed include (a) the fundamental nature of mass conservation and the role of detachment- and transport-limited processes in mass conservation equations, (b) the interaction between detachment- and transport-limitation in channels, (c) the role of hillslope erosion and soil properties and their interaction with channel processes, (d) the interactions with tectonics when applying these models at large scale, (e) depositional structures and implications for paleo-climatic interpretation, (f) engineering applications of these models, and (g) numerical issues in the computer implementations. This review is not a model comparison. However, many applications are at the boundaries of computer capabilities so a comparison of existing models is provided.
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    Annual Review of Earth and Planetary Sciences 33 (2005), S. 531-570 
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    Notes: The Earth has a radiogenic W-isotopic composition compared to chondrites, demonstrating that it formed while 182Hf (half-life 9 Myr) was extant in Earth and decaying to 182W. This implies that Earth underwent early and rapid accretion and core formation, with most of the accumulation occurring in Đ♯10 Myr, and concluding approximately 30 Myr after the origin of the Solar System. The Hf-W data for lunar samples can be reconciled with a major Moon-forming impact that terminated the terrestrial accretion process Đ♯30 Myr after the origin of the Solar System. The suggestion that the proto-Earth to impactor mass ratio was 7:3 and occurred during accretion is inconsistent with the W isotope data. The W isotope data is satisfactorily modeled with a Mars-sized impactor on proto-Earth (proto-Earth to impactor ratio of 9:1) to form the Moon at Đ♯30 Myr.
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    Annual Review of Earth and Planetary Sciences 33 (2005), S. 645-671 
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    Notes: The influence of surface orography on patterns of precipitation gives rise to some of the most pronounced climate gradients on Earth, and plays a fundamental role in the interaction between the atmosphere and the rest of the Earth System on a wide variety of time scales. The physical mechanisms involved comprise a rich set of interactions encompassing fluid dynamics, thermodynamics, and micron-scale cloud processes, as well as being dependent on the larger-scale patterns of the atmospheric general circulation. Investigations into orographic precipitation have pursued three parallel tracks of inquiry: observations, theory, and modeling. Significant advances have been made in each over the last few decades, and these are summarized and synthesized here. While many aspects of the basic mechanisms responsible for orographic precipitation have been understood, important issues remain unresolved. The sheer number of contributing processes, together with their convoluted interactions, make the quantitative prediction of precipitation in complex terrain a very hard task. However, while prediction of precipitation amounts for any given event may be difficult, various lines of evidence suggest that the patterns of orgraphic precipitation, even on scales of a few kilometers, are much more robust.
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    Annual Review of Earth and Planetary Sciences 10 (1982), S. 61-108 
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    Annual Review of Earth and Planetary Sciences 11 (1983), S. 241-268 
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    Annual Review of Earth and Planetary Sciences 33 (2005), S. 195-214 
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    Notes: Real-time seismology refers to a practice in which seismic data are collected and analyzed quickly after a significant seismic event, so that the results can be effectively used for postearthquake emergency response and early warning. As the technology of seismic instrumentation, telemetry, computers, and data storage facility advances, the real-time seismology for rapid postearthquake notification is essentially established. Research for early warning is still underway. Two approaches are possible: (a) regional warning and (b) on-site (or site-specific) warning. In (a), the traditional seismological method is used to locate an earthquake, determine the magnitude, and estimate the ground motion at other sites. In (b), the beginning of the ground motion (mainly P wave) observed at a site is used to predict the ensuing ground motion at the same site. An effective approach to on-site warning is discussed in light of earthquake rupture physics.
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    Annual Review of Earth and Planetary Sciences 33 (2005), S. 369-393 
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    Notes: Stable cratons and stable continental platforms are salient features of the Earth. Mantle xenoliths provide detailed data on deep structure. Cratonal lithosphere is about 200 km thick. It formed in the Archean by processes analogous to modern tectonics and has been stable beneath the larger cratons since that time. Its high viscosity, high yield strength, and chemical buoyancy protected it from being entrained by underlying stagnant lid convection and by subduction. Chemically buoyant mantle does not underlie platforms. Platform lithosphere has gradually thickened with time as convection waned as the Earth's interior cooled. The thermal contraction associated with this thickening causes platforms to subside relative to cratons. At present, the thickness of platform lithosphere is comparable to that of cratonal lithosphere.
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    Notes: The Ediacara biota (575Đ??542 Ma) marks the first appearance of large, architecturally complex organisms in Earth history. Present evidence suggests that the Ediacara biota included a mixture of stem- and crown-group radial animals, stem-group bilaterian animals, "failed experiments" in animal evolution, and perhaps representatives of other eukaryotic kingdoms. These soft-bodied organisms were preserved under (or rarely within) event beds of sand or volcanic ash, and four distinct preservational styles (Flinders-, Fermeuse-, Conception-, and Nama-style) profoundly affected the types of organisms and features that could be preserved. Even the earliest Ediacaran communities (575-565 Ma) show vertical and lateral niche subdivision of the sessile, benthic, filter-feeding organisms, which is strikingly like that of Phanerozoic and modern communities. Later biological and ecological innovations include mobility (〉555 Ma), calcification (550 Ma), and predation (〈549 Ma). The Ediacara biota abruptly disappeared 542 million years ago, probably as a consequence of mass extinction andor biological interactions with the rapidly evolving animals of the Cambrian explosion.
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    Annual Review of Earth and Planetary Sciences 33 (2005), S. 531-570 
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    Notes: The Earth has a radiogenic W-isotopic composition compared to chondrites, demonstrating that it formed while 182Hf (half-life 9 Myr) was extant in Earth and decaying to 182W. This implies that Earth underwent early and rapid accretion and core formation, with most of the accumulation occurring in Đ♯10 Myr, and concluding approximately Đ♯30 Myr after the origin of the Solar System. The Hf-W data for lunar samples can be reconciled with a major Moon-forming impact that terminated the terrestrial accretion process 30 Myr after the origin of the Solar System. The suggestion that the proto-Earth to impactor mass ratio was 7:3 and occurred during accretion is inconsistent with the W isotope data. The W isotope data is satisfactorily modeled with a Mars-sized impactor on proto-Earth (proto-Earth to impactor ratio of 9:1) to form the Moon at Đ♯30 Myr.
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    Annual Review of Earth and Planetary Sciences 8 (1980), S. 1-17 
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    Annual Review of Earth and Planetary Sciences 9 (1981), S. 385-413 
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    Annual Review of Earth and Planetary Sciences 33 (2005), S. 1-36 
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    Notes: This paper reviews the Precambrian history of atmospheric oxygen, beginning with a brief discussion of the possible nature and magnitude of life before the evolution of oxygenic photosynthesis. This is followed by a summary of the various lines of evidence constraining oxygen levels through time, resulting in a suggested history of atmospheric oxygen concentrations. Also reviewed are the various processes regulating oxygen concentrations, and several models of Precambrian oxygen evolution are presented. A sparse geologic record, combined with uncertainties as to its interpretation, yields only a fragmentary and imprecise reading of atmospheric oxygen evolution. Nevertheless, oxygen levels have increased through time, but not monotonically, with major and fascinating swings to both lower and higher levels.
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    Annual Review of Earth and Planetary Sciences 33 (2005), S. 163-193 
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    Notes: Weather and climate predictions are uncertain, because both forecast initial conditions and the computational representation of the known equations of motion are uncertain. Ensemble prediction systems provide the means to estimate the flow-dependent growth of uncertainty during a forecast. Sources of uncertainty must therefore be represented in such systems. In this paper, methods used to represent model uncertainty are discussed. It is argued that multimodel and related ensembles are vastly superior to corresponding single-model ensembles, but do not provide a comprehensive representation of model uncertainty. A relatively new paradigm is discussed, whereby unresolved processes are represented by computationally efficient stochastic-dynamic schemes.
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    Notes: Recent fossil discoveries from Early Cretaceous rocks of Liaoning Province, China, have provided a wealth of spectacular specimens. Included in these are the remains of several different kinds of small theropod dinosaurs, many of which are extremely closely related to modern birds. Unique preservation conditions allowed soft tissues of some of these specimens to be preserved. Many dinosaur specimens that preserve feathers and other types of integumentary coverings have been recovered. These fossils show a progression of integumentary types from simple fibers to feathers of modern aspect. The distribution of these features on the bodies of these animals is surprising in that some show large tail plumes, whereas others show the presence of wing-like structures on both fore and hind limbs. The phylogenetic distribution of feather types is highly congruent with models of feather evolution developed from developmental biology.
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    Notes: Ichthyosaurs were a group of Mesozoic marine reptiles that evolved fish-shaped body outlines. They are unique in several anatomical characters, including the possession of enormous eyeballs sometimes exceeding 25 cm and an enlarged manus with sometimes up to 20 bones in a single digit, or 10 digits per manus. They are also unique in that their biology has been studied from the perspective of physical constraints, which allowed estimation of such characteristics as optimal cruising speed, visual sensitivity, and even possible basal metabolic rate ranges. These functional inferences, although based on physical principles, obviously contain errors arising from the limitations of fossilized data, but are necessarily stronger than the commonly made inferences based on superficial correlations among quantities without mechanical or optical explanations for why such correlations exist.
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    Notes: We know that giant planets played a crucial role in the making of our Solar System. The discovery of giant planets orbiting other stars is a formidable opportunity to learn more about these objects, what their composition is, how various processes influence their structure and evolution, and most importantly how they form. Jupiter, Saturn, Uranus, and Neptune can be studied in detail, mostly from close spacecraft flybys. We can infer that they are all enriched in heavy elements compared to the Sun, with the relative global enrichments increasing with distance to the Sun. We can also infer that they possess dense cores of varied masses. The intercomparison of presently characterized extrasolar giant planets shows that they are also mainly made of hydrogen and helium, but that they either have significantly different amounts of heavy elements, have had different orbital evolutions, or both. Hence, many questions remain and need to be answered to make significant progress on the origins of planets. Pourquoi l'azur muet et l'espace insondable? Pourquoi les astres d'or fourmillant comme un sable? Arthur RimbaudĐ??Soleil et chair
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    Annual Review of Earth and Planetary Sciences 10 (1982), S. 109-128 
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    Annual Review of Earth and Planetary Sciences 11 (1983), S. 45-73 
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    Annual Review of Earth and Planetary Sciences 11 (1983), S. 195-214 
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    Annual Review of Earth and Planetary Sciences 11 (1983), S. 269-298 
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    Annual Review of Earth and Planetary Sciences 11 (1983), S. 299-327 
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    Annual Review of Earth and Planetary Sciences 12 (1984), S. 489-516 
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    Notes: Orogenic collapse is a process that transfers gravitational potential energy from regions of high potential energy to regions of lower potential energy. This transfer is classically considered to be accomplished by extension in the orogenic core and by synchronous shortening in foreland regions of the orogen. Not all extensional features in collisional mountain belts need, however, reflect orogenic collapse. Normal faulting, thrust faulting, and strike-slip faulting are all active in different parts of the Alps today and reflect complex local responses to ongoing Europe-Adria convergence. The Western Alps is the only area today where extension and shortening radial to orogen trend occur synchronously and where orogenic collapse may be an important process. Elsewhere in the Alps, normal faults are oriented at a high angle to orogen trend and were primarily active in Oligocene and Miocene time. Most present-day activity in the Central and Eastern Alps is on strike-slip faults that are accommodating lateral extrusion of material rather than orogenic collapse.
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  • 93
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    Palo Alto, Calif. : Annual Reviews
    Annual Review of Earth and Planetary Sciences 33 (2005), S. 133-161 
    ISSN: 0084-6597
    Source: Annual Reviews Electronic Back Volume Collection 1932-2001ff
    Topics: Geosciences , Physics
    Notes: The bulk of the Đ♯50-km-thick Martian crust formed at Đ♯4.5 Gyr B.P., perhaps from a magma ocean. This crust is probably a basaltic andesite or andesite and is enriched in incompatible and heat-producing elements. Later additions of denser basalt to the crust were volumetrically minor, but resurfaced significant portions of the Northern hemisphere. A significant fraction of the total thickness of the crust was magnetized prior to 4 Gyr B.P., with the magnetization later selectively removed by large impacts. Early large impacts also modified the hemispheric contrast in crustal thickness (the dichotomy), which was possibly caused by long-wavelength mantle convection. Subsequent Noachian modification of the crust included further impacts, significant fluvial erosion, and volcanism associated with the formation of the Tharsis rise. Remaining outstanding questions include the origin of the dichotomy and the nature of the magnetic anomalies.
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  • 94
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    Palo Alto, Calif. : Annual Reviews
    Annual Review of Earth and Planetary Sciences 33 (2005), S. 163-193 
    ISSN: 0084-6597
    Source: Annual Reviews Electronic Back Volume Collection 1932-2001ff
    Topics: Geosciences , Physics
    Notes: Weather and climate predictions are uncertain, because both forecast initial conditions and the computational representation of the known equations of motion are uncertain. Ensemble prediction systems provide the means to estimate the flow-dependent growth of uncertainty during a forecast. Sources of uncertainty must therefore be represented in such systems. In this paper, methods used to represent model uncertainty are discussed. It is argued that multimodel and related ensembles are vastly superior to corresponding single-model ensembles, but do not provide a comprehensive representation of model uncertainty. A relatively new paradigm is discussed, whereby unresolved processes are represented by computationally efficient stochastic-dynamic schemes.
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  • 95
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    Palo Alto, Calif. : Annual Reviews
    Annual Review of Earth and Planetary Sciences 8 (1980), S. 35-63 
    ISSN: 0084-6597
    Source: Annual Reviews Electronic Back Volume Collection 1932-2001ff
    Topics: Geosciences , Physics
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  • 96
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    Palo Alto, Calif. : Annual Reviews
    Annual Review of Earth and Planetary Sciences 8 (1980), S. 145-167 
    ISSN: 0084-6597
    Source: Annual Reviews Electronic Back Volume Collection 1932-2001ff
    Topics: Geosciences , Physics
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  • 97
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    Palo Alto, Calif. : Annual Reviews
    Annual Review of Earth and Planetary Sciences 8 (1980), S. 231-261 
    ISSN: 0084-6597
    Source: Annual Reviews Electronic Back Volume Collection 1932-2001ff
    Topics: Geosciences , Physics
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  • 98
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    Palo Alto, Calif. : Annual Reviews
    Annual Review of Earth and Planetary Sciences 8 (1980), S. 343-370 
    ISSN: 0084-6597
    Source: Annual Reviews Electronic Back Volume Collection 1932-2001ff
    Topics: Geosciences , Physics
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  • 99
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    Palo Alto, Calif. : Annual Reviews
    Annual Review of Earth and Planetary Sciences 9 (1981), S. 147-174 
    ISSN: 0084-6597
    Source: Annual Reviews Electronic Back Volume Collection 1932-2001ff
    Topics: Geosciences , Physics
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  • 100
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    Palo Alto, Calif. : Annual Reviews
    Annual Review of Earth and Planetary Sciences 9 (1981), S. 199-225 
    ISSN: 0084-6597
    Source: Annual Reviews Electronic Back Volume Collection 1932-2001ff
    Topics: Geosciences , Physics
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