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domingo, 20 de septiembre de 2015

NASA : NASA's LRO Discovers Earth's Pull is 'Massaging' our Moon .- NASA's Lunar Reconnaissance Orbiter (LRO) de la NASA descubre Tire de la Tierra está "masajeando" nuestra Luna

Hola amigos: A VUELO DE UN QUINDE EL BLOG., Gravedad de la Tierra ha influido en la orientación de miles de fallas que se forman en la superficie lunar como la luna se encoge, de acuerdo con los nuevos resultados de NASA's Lunar Reconnaissance Orbiter (LRO) spacecraft.
More information...............
 
Earth's gravity has influenced the orientation of thousands of faults that form in the lunar surface as the moon shrinks, according to new results from NASA's Lunar Reconnaissance Orbiter (LRO) spacecraft.
gif of moon in orbit around earth
The gravitational forces the Moon and Sun exert are responsible for Earth’s rising and falling tides. Earth’s gravity also exerts forces on the Moon in the form of solid body tides that distort its shape. The Moon is slowly receding away from Earth and forces build as the Moon’s tidal distortion diminishes with distance and its rotation period slows with time. These tidal forces combined with the shrinking of the Moon from cooling of its interior have influenced the pattern of orientations in the network of young fault scarps.
Credits: NASA/LRO/Arizona State University/Smithsonian Institution
 
lunar topography with arrows
Thousands of young, lobate thrust fault scarps have been revealed in Reconnaissance Orbiter Camera images (LROC). Lobate scarps like the one shown here are like stair-steps in the landscape formed when crustal materials are pushed together, break and are thrust upward along a fault forming a cliff. Cooling of the still hot lunar interior is causing the Moon to shrink, but the pattern of orientations of the scarps indicate that tidal forces are contributing to the formation of the young faults.
Credits: NASA/LRO/Arizona State University/Smithsonian Institution
 
lunar map showing movement over large areas
The map shows the locations of over 3,200 lobate thrust fault scarps (red lines) on the Moon. The black double arrows show the average orientations of the lobate scarps sampled in areas with dimensions of 40° longitude by 20° latitude and scaled by the total length of the fault scarps in the sampled areas. The pattern of the black double arrows (orientation vectors) indicates that the fault scarps do not have random orientations as would be expected if the forces that formed them were from global contraction alone. Mare basalt units are shown in tan.
Credits: NASA/LRO/Arizona State University/Smithsonian Institution
 
lunar topography in false color
A prominent lobate fault scarp in the Vitello Cluster is one of thousands discovered in Lunar Reconnaissance Orbiter Camera images (LROC). Topography derived from the LROC Narrow Angle Camera (NAC) stereo images shows a degraded crater has been uplift as the fault scarp has formed (blues are lower elevations and reds are higher elevations). Boulders in the crater have aligned in rows that parallel the orientation of the fault scarp.
Credits: NASA/LRO/Arizona State University/Smithsonian Institution
 
lunar topography from above and an angle
A nadir (top) and perspective view (bottom) of a prominent lobate fault scarp in the Vitello Cluster, one of thousands discovered in Lunar Reconnaissance Orbiter Camera images (LROC). In the perspective view, the Narrow Angle Camera (NAC) image is draped over topography derived from NAC stereo images. A degraded crater has been uplift as the fault scarp has formed. Boulders in the crater have aligned in rows that parallel the orientation of the fault scarp.
Credits: NASA/LRO/Arizona State University/Smithsonian Institution
 
In August, 2010, researchers using images from LRO's Narrow Angle Camera (NAC) reported the discovery of 14 cliffs known as "lobate scarps" on the moon's surface, in addition to about 70 previously known from the limited high-resolution Apollo Panoramic Camera photographs. Due largely to their random distribution across the surface, the science team concluded that the moon is shrinking.
These small faults are typically less than 6.2 miles (10 kilometers) long and only tens of yards or meters high. They are most likely formed by global contraction resulting from cooling of the moon's still hot interior. As the interior cools and portions of the liquid outer core solidify, the volume decreases; thus the moon shrinks and the solid crust buckles.
Now, after more than six years in orbit, the Lunar Reconnaissance Orbiter Camera (LROC) has imaged nearly three-fourths of the lunar surface at high resolution, allowing the discovery of over 3,000 more of these features. These globally distributed faults have emerged as the most common tectonic landform on the moon. An analysis of the orientations of these small scarps yielded a surprising result: the faults created as the moon shrinks are being influenced by an unexpected source—gravitational tidal forces from Earth.
Global contraction alone should generate an array of thrust faults with no particular pattern in the orientations of the faults, because the contracting forces have equal magnitude in all directions. "This is not what we found," says Smithsonian senior scientist Thomas Watters of the National Air and Space Museum in Washington. "There is a pattern in the orientations of the thousands of faults and it suggests something else is influencing their formation, something that's also acting on a global scale -- 'massaging' and realigning them." Watters is lead author of the paper describing this research published in the October issue of the journal Geology.
The other forces acting on the moon come not from its interior, but from Earth. These are tidal forces. When the tidal forces are superimposed on the global contraction, the combined stresses should cause predictable orientations of the fault scarps from region to region. "The agreement between the mapped fault orientations and the fault orientations predicted by the modeled tidal and contractional forces is pretty striking," says Watters.
"The discovery of so many previously undetected tectonic features as our LROC high-resolution image coverage continues to grow is truly remarkable," said Mark Robinson of Arizona State University, coauthor and LROC principal investigator. "Early on in the mission we suspected that tidal forces played a role in the formation of tectonic features, but we did not have enough coverage to make any conclusive statements. Now that we have NAC images with appropriate lighting for more than half of the moon, structural patterns are starting to come into focus."
The fault scarps are very young – so young that they are likely still actively forming today. The team's modeling shows that the peak stresses are reached when the moon is farthest from Earth in its orbit (at apogee). If the faults are still active, the occurrence of shallow moonquakes related to slip events on the faults may be most frequent when the moon is at apogee. This hypothesis can be tested with a long-lived lunar seismic network. 
"With LRO we've been able to study the moon globally in detail not yet possible with any other body in the solar system beyond Earth, and the LRO data set enables us to tease out subtle but important processes that would otherwise remain hidden," said John Keller, LRO Project Scientist at NASA's Goddard Space Flight Center, Greenbelt, Maryland.
Launched on June 18, 2009, LRO has collected a treasure trove of data with its seven powerful instruments, making an invaluable contribution to our knowledge about the moon. LRO is managed by NASA's Goddard Space Flight Center in Greenbelt, Maryland, under the Discovery Program, managed by NASA's Marshall Space Flight Center in Huntsville for the Science Mission Directorate at NASA Headquarters in Washington, DC.
Nancy Neal-Jones / William Steigerwald
NASA Goddard Space Flight Center, Greenbelt, Maryland
301-286-0039 / 6-5017
nancy.n.jones@nasa.gov / william.a.steigerwald@nasa.gov
Last Updated: Sep. 15, 2015
Editor: Karl Hille
Tags:  Goddard Space Flight Center, LRO (Lunar Reconnaissance Orbiter), Moons, Solar System
 NASA
Guillermo Gonzalo Sánchez Achutegui
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