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Kaguya-013-20071128_kaguya_tc02_04.jpgDyson Crater (2)74 visitenessun commentoMareKromium
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APOLLO_12_AS_12-57-8444_HR-c.jpgAS 12-57-8444 (c - extra-detail mgnf) - Soil surface disturbed by the LM descent engine exhaust (coloring: Lunexit)74 visiteLa nostra extra-magnificazione (alla quale abbiamo aggiunto un aumento del contrasto ed un'ulteriore, ancorchè modesta, messa a fuoco) non può risolvere al 100% il "mistero" del dettaglio controverso (battezzato la "lampadina") ma ci può essere di aiuto per appurare, se non altro, la sua sostanziale non linearità ed asimmetricità: due elementi, questi, i quali ci fanno definitivamente propendere per l'origine naturale del particolare. Ad ogni modo, considerando l'estensione del quadro ripreso nel full-frame e sapendo che il sassolino più grande dell'intero quadro misura circa 1,4 cm, abbiamo stimato la dimensione dell'ipotetica lampadina nell'ordine dei 0,2-0,4 mm.
Ed ora attendiamo i Vostri commenti al riguardo.MareKromium
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LRO-1002-392723-MainCabaeus_full.jpgLCROSS Impact Location74 visitenessun commentoMareKromium
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LRO-2503-Mare_Moscoviense.jpgMare - Highlands Boundary in Mare Moscoviense74 visiteMare Moscoviense: a "Window" to the Lunar Far-Side Volcanism
It's clear from looking at pictures of the Moon that the Near-Side and the Far-Side are very different from a geologic standpoint.
The darker, basaltic mare deposits dominate the Near-Side, whereas the Far-Side is dominated by bright deposits of anorthosite thought to be remnants of the Moon's original crust. Mare Moscoviense is one of the few (and also the largest) deposits of mare basalts on the Lunar Far-Side.
Why are there so many mare basalts on the Near-Side, but so few on the Far-Side? Lunar scientists simply don't know the answer to that question. One idea is that the Far-Side crust is simply thicker than the near side crust, and rising basaltic magma simply solidified before it was able to push through the thicker Far-Side crust. That's where Moscoviense comes in. We know enough about the Moscoviense Region from previous missions that we have a well-defined set of questions that potential future missions might be able to answer. For example, the Lunar Prospector mission showed that there are high concentrations of thorium in the Moscoviense Basin. Thorium acts as a tracer for the Lunar KREEP (Potassium - K -, Rare Earth Elements and Phosphorus) geochemical component found in abundance on the Near-Side but not on the Far-Side.
Understanding the extent and distribution of thorium in the basin may tell us about the global distribution of the Lunar KREEP component and thus the evolution of the Lunar Mantle. We also know from the Clementine mission that the Moscoviense basalts are rich in both Iron and Titanium. Since basalts form by partial melting of the Lunar Mantle, sampling Moscoviense basalts provides lunar scientists with vital insights into how the Lunar Mantle on the Far-Side differs from the Near-Side one, which in turn would help us to learn why mare basalts are so much rarer on the Far-Side and provide key insights about the formation of all of the terrestrial planets, including Mars and Earth.
For these reasons, a Constellation Program region of interest is located within Mare Moscoviense. The region is at the edge of Moscoviense, allowing explorers to collect samples from both the mare basalts and the surrounding highlands terrain during their traverses.
The materials at the edge of the basin provide important insights into the formation of the Moscoviense Basin itself. By exploring and sampling the Moscoviense Region, we would date the basalt flows and definitively determine their composition. This sampling would let us determine how Moscoviense basalts differ from the near side basalts sampled during Apollo. Age-dating Moscoviense basalts also provides important insights into the history of lunar volcanism by determining whether the Moscoviense basalts are older or younger than Near-Side basalts.
While the scientific goals of exploring the Moscoviense Region are certainly important, no less important is access to key lunar resources. The lunar regolith (the broken-up rocks and impact products that make up the first 10 meters or so of the Lunar Surface) in this region is derived in part from the local titanium-rich Moscoviense basalts. This regolith material could be used for a variety of vital purposes, including the construction of human habitats, radiation shielding, or as feedstock for local resource utilization.
Taking a longer view, Titanium is an important industrial material on Earth, and it will be very important for indigenous lunar industrial development.MareKromium
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LRO-2500-Epigenes_A_Crater-1.jpgEpigenes A74 visiteA plethora of Boulders surrounds braided flows of impact melt along the Inner Wall of the Crater Epigenes A. As the melt moves toward the Crater Floor (direction indicated by white arrow), the flow buries and moves boulders.
Epigenes A is an about 18-Km-diameter Impact Crater located at 66,9° North and 0,3° West, on the Rim of crater W. Bond.
(this NAC image is 540 meters wide)MareKromium
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LRO-2500-Marius_Crater~0.jpgLandslides or unusual Surface-decoloration in Marius Crater? (Natural Colors; credits: Dr Paolo C. Fienga - Lunexit Team)74 visiteGrazie alla nostra Grande Amica e Partner Elisabetta Bonora, da oggi "Lunar Explorer Italia" è presente ed accessibile anche su Twitter.
Il nostro (e Vostro!) link - comunque già indicato nei "Links Suggeriti" nella Front Page di TruePlanets (sulla Dx) - è questo: http://twitter.com/lunexit .
Perchè questa "presenza" ulteriore?
Semplice, in un Mondo laddove la divulgazione della stupidità sembra costituire un trend in ascesa continua, noi (e Voi!) stiamo cercando di controbilanciare questa - orribile - tendenza mediante la Divulgazione della Ricerca, della Passione e, con tutti i nostri limiti, della Scienza.
Dalla Luna all'Infinito, naturalmente...
Dr Paolo C. Fienga - Lunar Explorer Italia
Presidente e Socio FondatoreMareKromium
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APOLLO 4 AS 04-01-603.jpgAS 04-01-603 - The "Blue Planet" in transit (6)73 visitenessun commento
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14-Vallis Schroteri.jpgVallis Schroteri and Schiaparelli Crater73 visiteCaption NASA originale:"Lunar Orbiter 4 image showing Vallis Schroteri, the sinuous valley at the upper right. The large crater at the lower left is Schiaparelli, approximately 22 Km across. The very edge of Heredotus crater can be seen at the middle right of the frame, and the small crater towards the lower right is Herodotus-A. North is up (Lunar Orbiter 4, frame 157-H3)".
Location & Time Information
Date/Time (UT): 1967-05-22 T 18:01:16
Distance/Range (km): 2670
Central Latitude/Longitude (deg): +13.36/303.73
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Triesnecker-02.jpgTriesnecker (3) - detail mgnf73 visitenessun commento
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14-De Gasparis Crater.jpgDe Gasparis Crater73 visiteDe Gasparis is a small to medium sized crater 30 Km in diamater located on the western flank of Mare Humorum. The rim of the crater is worn and eroded. The interior has, at some point, been flooded by lava and sits around 0,8 Km below the surrounding surface. The crater is intersected by a number of rimae including, running from top-left to lower-right of the crater, a part of the 93 Km long Rimae De Gasparis.
Due to the consistent depth of the rimae it evidently formed after the crater and is possibly associated with the tectonic activity which saw the infilling of the crater.
The crater is named after the Italian Astronomer Annibale de Gasparis (1819-1892, director of the observatory in Naples, Italy and discoverer of 9 asteroids). Along with the crater and rimae, asteroid 4279 is also named in his honour.
The image represents raw data and no flat field or other corrections have been applied.
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16-Lichtenberg Crater.jpgLichtenberg Crater (HR)73 visiteAn image of the prominent crater Lichtenberg with a diameter of 20 Km. The crater shows a 1300 mt height difference between crater floor and surrounding lava plain. The actual target of this observation was the 'ghost' crater on the lower left of Lichtenberg. It is almost hidden by overflown lava from Oceanus Procellarum in which it is located. This area is of high geological interest and it was selected for the study of the most recent lunar volcanism. It is thought to contain the youngest basalts on the Lunar Surface, with an age of about 1000 MY. Recent data show that lunar volcanism was active for at least 2000 MY from 4000 MY ago, ceasing at about 2000 MY. In Oceanus Procellarum, it is thought that these basalts are the youngest basalts on the lunar surface with an age of less than 1000 MY. This should be compared with the age of the Moon at about 4500 MY. This crater is named after the German physicist Georg Christoph Lichtenberg (1742-1799) who was professor at the newly formed Goettingen University.
Nota: a nostro parere, questa caption ESA è - sostanzialmente - del tutto incomprensibile ed anche errata. Nel momento in cui si sostiene, infatti, che il vulcanismo lunare è cessato da svariate centinaia di milioni di anni (o anche di più), implicitamente si dice che alcuni grandissimi Astronomi della nostra Storia, da Galileo a Flammarion (i quali hanno assistito a possibili eventi vulcanici lunari classificati come TLP nel famoso NASA Technical Report R-277), erano e sono, in realtà, dei "visionari".
Triste, come sempre; molto triste.
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The Moon - Near Side - Galileo.JPGThe "Near-Side" of the Moon, from Galileo73 visitenessun commento
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