Earth-Moon system

The much-closer Moon would have had a greater influence on the tidal rise and fall of the oceans. At the moment, the mid-ocean tidal rise and fall far removed from the land masses is of order 1 m but if the Moon had been formed at a distance of around 40 000 km the tidal variation would have been of the order 100-1000 m. Large regions of the Earth s surface would have had a refreshed water supply every 4 h in the extreme cases of the model. Only well inland on the early land masses would there have been a dry environment, perhaps with fresh water replenishment. The early ideas of Darwin called for a Tittle warm pool to act 

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The assignment of the earth/moon system to one precursor nebular reservoir, and meteorites to a second, while still logically possible, was shown experimentally to be unnecessary by Thiemens and coworkers (reading list). In the early 1980s these workers studied isotope fractionation during the synthesis of ozone from molecular oxygen in an electric discharge operated at low pressure. The product ozone was... 

SNC-meteorites have an average 8 0-value of 4.3%c, which is distinctly lower than the 5.5%c value for the Earth-Moon system (Clayton and Mayeda 1996 Franchi... 

Hartmann, W. K., Ryder, G., Dones, L. and Grinspoon, D. (2000) The time-dependent intense bombardment of the primordial Earth/Moon system. In Origin of the Earth and Moon, eds. Canup, R. M. and Righter, K. Tucson University of Arizona Press, pp. 493-512. 

Taylor, S. R., Pieters, . M. and MacPherson, G. J. (2006a) Earth-Moon system, planetary science, and lessons learned. In New Views of the Moon, Reviews in Mineralogy and Geochemistry 60, eds. Jolliff, B. L., Wieczorek, M. A., Shearer, . K. and Neal, C. R. Washington, D.C. Mineralogical Society of America and Geochemical Society, pp. 657-704. 

A significant aspect of skeletal growth in corals is the existence of an internal calendar where daily, seasonal, and annual records are kept on file in the form of individual or series of bands. The band thicknesses within a species are environmentally controlled. The number of bands per year in fossil corals has been used in studies on the Earth-Moon system, i.e. effect of tidal friction on number of days per year336. ... 

Floran R. J., Caulfield J. B. D., Harlow G. E., and Prinz M. (1978) Impact origin for the Simondium, Pinnaroo, and Hainholz mesosiderites imphcations for impact processes beyond the Earth—Moon system. Proc. Lunar Planet. Sci. Conf. 9, 1083-1114. 

Co-accretion. This theory proposes that the Earth and Moon simply accreted side by side. The difficulty with this model is that it does not explain the angular momentum of the Earth-Moon system, nor the difference in density, nor the difference in volatile depletion (Taylor, 1992). 

Canup R. M. and Agnor C. (1998) Accretion of terrestrial planets and the earth-moon system. In Origin ofthe Earth and Moon, LPI Contribution No. 597 Lunar and Planetary Institute, Houston, pp. 4-7. 

Ringwood A. E. (1990) Earhest history of the Earth-Moon system. In Origin of the Earth (eds. A. E. Newsom and J. H. Jones). Oxford University Press, Oxford, pp. 101-134. 

Miinker C., Pfander J. A., Weyer S., Biichl A., Kleine T., and Mezger K. (2003) Evolution of planetary cores and the earth-moon system from Nb/Ta systematics. Science 30, 84-87. 

Ohtani E., Yurmoto H., Segawa T., and Kato T. (1995) Element partitioning between MgSi03 perovskite, magma, and molten iron constraints for the earliest processes of the Earth-Moon system. In The Earth s Central Part Its Structure and Dynamics (ed. T. Yukutake). Terra Scientific, Tokyo, Japan, pp. 287-300. 

Wanke H. and Dreibus G. (1982) Chemical and isotopic evidence for the early history of the Earth—Moon system. In Tidal Friction and the Earth s Rotation (eds. P. Brosche and J. Sundermann). Springer, Berlin, pp. 322—344. 

Jupiter, and Saturn. These planets and the sun also perturb the moon s orbit around the Earth— Moon system s center of mass. The use of mathematical series for the orbital elements as functions of time can accurately describe perturbations of the orbits of solar system bodies for limited time intervals. For longer intervals, the series must be recalculated. 

As accurately as these calculations can be made, however, the behavior of celestial bodies over long periods of time cannot always be determined. For example, the perturbation method has so far been unable to determine the stability either of the orbits of individual bodies or of the solar system as a whole for the estimated age of the solar system. Studies of the evolution of the Earth-Moon system indicate that the Moon s orbit may become unstable, which will make it possible for the Moon to escape into an independent orbit around the Sun. Recent astronomers have also used the theory of chaos to explain irregular orbits. 

In summary, as a result of the Martian meteorites, we know more about the noble gases on Mars than about those on any planet besides Earth. As our knowledge of Martian noble gases grows, we continue to find results that are unexpected, and, at the moment, inexplicable, providing a valuable check for models that we devise based on our more detailed knowledge of the Earth-Moon system. 

Would the journey be made more difficult with the gravitational effect of a third planetary body placed midway between the Earth and the moon Where is the center of mass for the Earth-moon system Arlin Anderson notes that the moon s mass is about 1/80 of the Earth s, and the moon is almost 240,000 miles away. Therefore, the center of mass of the Earth-moon system is 3,000 miles from the center of the Earth, or 1,000 miles below the Earth s surface I am interested in hearing from readers with additional insight into how humans could efficiently climb the long ladder postulated in this problem. 

Still, the Earth s mantle is more oxidized than the other solar system bodies for which we have information from samples, the asteroid Vesta, the Moon, and Mars. The Earth s mantle most likely became oxidized during its accretion (for review see Ref. [52]). The climax was the collision of a Mars-sized body with the Protoearth that left the present Earth-Moon system in its wake. During this event (and after subsequent asteroid impacts) metallic iron mixed into the mantle and consumed hydrogen equivalent to that in the present oceans. A comparable amount of hydrogen was consumed making ferric iron in the mantle. 

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