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| Risultati della ricerca nelle immagini - "landscape" |
006-Ceres.jpg1-Ceres (natural colors, from HST - credits: NASA/ESA et al.)53 visiteThe Hubble image of Ceres on the reveals bright and dark regions on the asteroid's surface that could be topographic features, such as craters, and/or areas containing different surface material. Large impacts may have caused some of these features and potentially added new material to the landscape. The Texas-sized asteroid holds about 30 to 40% of the mass in the Asteroid Belt.
Ceres' round shape suggests that its interior is layered like those of terrestrial planets such as Earth. The asteroid may have a rocky inner core, an icy mantle, and a thin, dusty outer crust. The asteroid may even have water locked beneath its surface. It is approx. 590 miles (950 Km) across and was the first asteroid discovered in 1801.
The observation was made in visible and ultraviolet light between December 2003 and January 2004 with the HST Advanced Camera for Surveys. The color variations in the image show either a difference in texture or composition on Ceres' surface.
Astronomers need the close-up views of the Dawn spacecraft to determine the characteristics of these regional differences.
MareKromium
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30-Doradus.jpg30 Doradus and R-13652 visiteThe massive, young stellar grouping, called R136, is only a few million years old and resides in the 30 Doradus Nebula, a turbulent star-birth region in the Large Magellanic Cloud (LMC), a satellite galaxy of our Milky Way. Many of the stars are among the most massive known. Several of them are over 100 times more massive than our Sun. These hefty stars are destined to become supernovae in a few million years.
The image, taken by Hubble's Wide Field Camera 3, spans about 100 light-years. The nebula is close enough to Earth that Hubble can resolve individual stars, giving astronomers important information about the stars' birth and evolution.
The brilliant stars are carving deep cavities in the surrounding material by unleashing a torrent of ultraviolet light, and hurricane-force stellar winds (streams of charged particles), which are etching away the enveloping hydrogen gas cloud in which the stars were born. The image reveals a fantasy landscape of pillars, ridges, and valleys, as well as a dark region in the center that roughly looks like the outline of a holiday tree. Besides sculpting the gaseous terrain, the brilliant stars can also help create a successive generation of offspring. When the winds hit dense walls of gas, they create shocks, which may be generating a new wave of star birth.
The movement of the LMC around the Milky Way may have triggered the massive cluster's formation in several ways. The gravitational tug of the Milky Way and the companion Small Magellanic Cloud may have compressed gas in the LMC. Also, the pressure resulting from the LMC plowing through the Milky Way's halo may have compressed gas in the satellite. The cluster is a rare, nearby example of the many super star clusters that formed in the distant, early universe, when star birth and galaxy interactions were more frequent. Previous Hubble observations have shown astronomers that super star clusters in faraway galaxies are ubiquitous. The LMC is located 170,000 light-years away and is a member of the Local Group of Galaxies, which also includes the Milky Way.
The Hubble image was taken at infrared wavelengths (1.1 microns and 1.6 microns). Hubble sees through the dusty nebula, revealing many stars that cannot be seen in visible light. The large bright star just above the center of the image is in the 30 Doradus nebula. The Hubble observations of 30 Doradus were made October 20-27, 2009.MareKromium
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56-Luna13 - Panorama-02.jpgLunik 13: Oceanus Procellarum (2)132 visiteThe Luna 13 spacecraft was launched toward the Moon from an Earth-orbiting platform and accomplished a soft landing on December 24, 1966, in the Region of "Oceanus Procellarum". The petal encasement of the spacecraft was opened, antennas were erected, and radio transmissions to Earth began 4 minutes after the landing. On December 25 and 26, 1966, the spacecraft television system transmitted panoramas of the nearby lunar landscape at different sun angles. Each panorama required approximately 100 minutes to transmit. The spacecraft was equipped with a mechanical soil-measuring penetrometer, a dynamograph, and a radiation densitometer for obtaining data on the mechanical and physical properties and the cosmic-ray reflectivity of the lunar surface. It is believed that transmissions from the spacecraft ceased before the end of December 1966.
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APOLLO 16 AS 16-5006 (1).jpgAS 16-5006 - Details of King Crater (1)52 visiteHere is an enlarged vertical view of more flow lobes inside King Crater. Fine lineations radial to King are prominent in the ejecta blanket behind (South-East of) the lobate fronts. The term "deceleration lobe" has been applied because the lobes occur only where the ejecta slowed down and came to rest on slopes that face toward King. They resemble terrestrial rock avalanche deposits that came to rest after climbing a small slope. Some lobes overlap each other outward like shingles.
The sketch (2) shows what would probably be seen in a cutaway view. The arrow shows the direction of movement of the ejecta over the old landscape.
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AuroraBorealis-Alaska.jpgAurora over Alaska55 visiteCaption NASA:"Higher than the highest mountain, higher than the highest airplane, lies the realm of the aurora. Aurora rarely reach below 60 Km, and can range up to 1000. Aurora light results from solar shockwave causing energetic electrons and protons to striking molecules in the Earth's atmosphere. Frequently, when viewed from space, a complete aurora will appear as a circle around one of the Earth's magnetic poles. The above digitally enhanced photograph was taken in 2005 January shows a spectacular aurora borealis above the frozen landscape of Bear Lake, Alaska, USA.
The above image was voted Wikipedia Commons Picture of the Year for 2006".
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Chaotic_Terrain-Cerberus_Fossae.jpgChaotic Terrain in Cerberus Fossae (Original NASA/JPL/ASU b/w Frame)85 visiteNella Regione Marziana conosciuta con il tenebroso nome di "Cerberus Fossae" possiamo vedere, grazie a questa splendida 'veduta orbitale' ottenuta dalla Sonda NASA "2001 - Mars Odyssey", un terreno ricco di intriganti e variegati rilievi.
Qualche cratere relativamente recente (che reca segni di wind-streaks scuri) e qualcuno pi antico e semi-sepolto; delle colline che sembrano poggiare sopra un "basamento" e poi - forse una delle caratteristiche pi inquietanti di questo scorcio di Marte - dei profondi e scoscesi crepacci frastagliati.
Questo tipo di zona viene definito "chaos" e si tratta di un'area che stata - letteralmente - privata di sostegno sotterraneo e che quindi "crollata su s stessa" (---> "Chaos" is typically interpreted to be a collapse terrain; it is the blocky landscape after the transport and removal of subsurface support).
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Chaotic_Terrain-Jani_Chaos-PIA03200.jpgFeatures of Iani Chaos (Original NASA/2001 Mars Odyssey Orbiter b/w Frame)52 visitePiccolo promemoria: quando si parla di "chaos terrain", si tratta di un'area che stata - letteralmente - privata di sostegno sotterraneo e che quindi "crollata su se stessa" (---> "Chaos" is typically interpreted to be a collapse terrain; it is the blocky landscape after the transport and removal of subsurface support).
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Collapse_Features-Trough-Cerberus_Fossae-00.jpgFeatures of Cerberus Fossae (Original NASA/MGS/MSSS CTX b/w Frame)76 visiteCaption originale:"This MGS-MOC image shows a landscape in the Eastern Cerberus Region that was scoured by catastrophic Floods, and later cut by a deep, dark-walled Trough. The Trough is radial to the Elysium Volcanic Region, and formed along Faults in the Bedrock".
Location near: 15,7 North Lat. and 196,6 West Long.
Image width: ~3 Km (~1,9 mi)
Illumination from: lower left
Season: Northern Winter
Nota: l'immagine davvero spettacolare ed anche prodiga di dettagli (grazie ad un'eccellente definizione); purtroppo, per, non riusciamo a vedere bene se, nelle parti pi in ombra - e forse anche pi profonde - del crepaccio che lacera la porzione orientale della Regione di Cerberus, si nasconde qualcosa di particolare, oltre alle "dunette sinuose" (una forma affine ai Side-Winders di Meridiani Planum).
Cerchiature Verdi: agevole notare la presenza di ampie chiazze scure su buona parte del SOLO versante occidentale (Sx) del crepaccio le quali, secondo noi, NON sono assolutamente delle ombre. E' del tutto ovvio che la reale natura delle "macchie" sia indefinibile da questa altezza (380 Km) e con questa definizione, ma l'ipotesi che si tratti di "affioramenti di umidit", ovvero di "seeps" molto estesi ed in corso di sviulppo, o magari di aree ricoperte da una sorta di vegetazione indigena (magari muschi e licheni?), come gi pensano in molti, non ci sembrano tanto irrealistiche.
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Craters-Isabella_Crater-PIA00480.jpgIsabella Crater (possible Natural Colors; credits: Dr Paolo C. Fienga - Lunexit Team)53 visiteCrater Isabella, with a diameter of approx. 175 Km (such as about 108 miles), seen in this MRI (Magellan Radar Image), is the second largest Impact Crater on Venus.
The feature is named in honor of the 15th Century Queen of Spain, Isabella of Castile. Located at 30 South Latitude and 204 East Longitude, the Crater has two extensive flow-like structures extending to the South and to the S/E.
The end of the Southern Flow partially surrounds a pre-existing 40 Km (approx. 25 mile) circular Volcanic Shield.
The South-Eastern Flow shows a complex pattern of Channels and Flow Lobes, and is overlain at its South-Eastern tip by deposits from a later approx. 20 Km (about 12 mile) diameter Impact Crater, Cohn (for Carola Cohn, Australian artist, 1892-1964).
The extensive Flows, unique to Venusian Impact Craters, are a continuing subject of study for a number of Planetary Scientists. It is thought that the Flows may consist of "Impact Melt", suc as rock melted by the intense heat released in the impact explosion. An alternate hypothesis invokes "Debris Flows", which may consist of clouds of hot gases and both melted and solid rock fragments that race across the landscape during the impact event.
That type of Emplacement Process is similar to that which occurs in violent eruptions on Earth, such as the 1991 Mount Pinatubo eruption in the Philippines.MareKromium
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Craters-Unnamed_Craters-ESP_031292_1295-PCF-LXTT-IPF.jpgUnnamed Craters in Hellas Planitia (Absolute Natural Colors; credits for the additional process. and color.: Dr Paolo C. Fienga/Lunar Explorer Italia/Italian Planetary Foundation)70 visiteIn this frame, taken by the NASA - Mars Reconnaissance Orbiter on March, 30, 2013 and showing us a small portion of the Southern Martian Region known as Hellas Planitia, we can see - litterally lost in a "Sea" of Sand that has also been heavily marked by the passage of a countless number of Dust Devils - two relatively small Unnamed Impact Craters which are going through two very different (and very distant, in terms of time) moments of their evolution.
Barely visible, on the left (Sx) side of the picture, there is an extremely old and now almost completely "Buried Impact Crater", whose Rim, however, can still be discerned from the surrounding landscape; on the right (Dx) side of the frame, instead, a way more recent Unnamed Impact Crater that shows a very well defined (and therefore - of course, always relatively speaking - "fresh") Rim, with signs of a Landslide, that has occurred on its Inner Southern Slope, and also with what appears to be just a hint of a light-colored Windstreak on its Northern Outer Rim. Also a few Gullies can be spotted in several locations of the Inner Slopes of the Crater (particularly on its North-facing Inner Rim and Slope).
Mars Local Time: 14:37 (Early Afternoon)
Coord. (centered): 50,284 South Lat. and 54,671 East Long.
Spacecraft altitude: 255,9 Km (such as about 158,913 miles)
Original image scale range: 51,2 cm/pixel (with 2 x 2 binning) so objects ~ 1 mt and 54 cm across are resolved
Map projected scale: 50 cm/pixel
Map projection: EQUIRECTANGULAR
Emission Angle: 1,6
Phase Angle: 42,2
Solar Incidence Angle: 41 (meaning that the Sun was about 49 above the Local Horizon at the time the picture was taken)
Solar Longitude: 292,3 (Northern Winter - Southern Summer)
Credits: NASA/JPL/University of Arizona
Additional process. and coloring: Lunar Explorer Italia
This picture (which has been cropped from a NASA - Original Mars Reconnaissance Orbiter NON-Map Projected CTX b/w frame identified by the serial n. ESP_031292_1295) has also been additionally processed and then colorized in Absolute Natural Colors (such as the colors that a human eye would actually perceive if someone were onboard the NASA - Mars Reconnaissance Orbiter and then looked down, towards the Surface of Mars - Region of Hellas Planitia), by using an original technique created - and, in time, dramatically improved - by the Lunar Explorer Italia Team.MareKromium
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Craters-Victoria_Crater-PIA12167.jpgVictoria Crater (Natural Colors; credits: Lunexit)56 visiteThis image of Victoria Crater in the Meridiani Planum Region of Mars was taken by the High Resolution Imaging Science Experiment (HiRISE) camera on NASA's Mars Reconnaissance Orbiter at more of a sideways angle than earlier orbital images of this feature.
The camera pointing was 22 East of straight down, yielding a view comparable to looking at the landscape out an airplane window. East is at the top. The most interesting exposures of geological strata are in the steep walls of the Crater, difficult to see from straight overhead.
Especially prominent in this oblique view is a bright band near the top of the Crater wall.
Earlier HiRISE images of Victoria Crater supported the exploration of this Crater by NASA's Opportunity Rover and contributed to joint scientific studies. Opportunity explored the Rim and interior of this 800-meter-wide (about 0,5-mile-wide) Crater from September 2006 through August 2008.
The Rover's on-site investigations indicated that the bright band near the top of the Crater wall was formed by diagenesis (chemical and physical changes in sediments after deposition). The bright band separates bedrock from the material displaced by the impact that dug the Crater.
This view is a cutout from a HiRISE exposure taken on July 18, 2009. Some of Opportunity's Tracks are still visible to the North of the Crater (left side of this cutout).
Full-frame images from this HiRISE observation, catalogued as ESP_013954_1780, are at http://hirise.lpl.arizona.edu/ESP_013954_1780.
The full-frame image is centered at 2,1 South Latitude and 354,5 East Longitude. It was taken at 2:31 p.m. Local Mars Time. The scene is illuminated from the West with the Sun about 49 above the Local Horizon (therefore the S.I.A. was about 41).MareKromium
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Dione-PIA07745-1.jpgDione's horizon - HD (1)53 visiteOriginal caption:"As it departed its encounter with Saturn's moon Dione, Cassini sailed above an unreal landscape blasted by impacts. The rising Sun throws craters into sharp contrast and reveals steep crater walls.
At the far right, a medium-sized crater is bisected by a fracture, revealing a cross section of the impact site.
The seven clear-filter images in this mosaic were taken with the Cassini spacecraft narrow-angle camera on Oct. 11, 2005, at distances ranging from of 21.650 to 25.580 Km (about 13.450 to 15.890 miles) from Dione and at a Sun-Dione-spacecraft, or phase, angle of 154. Resolution in the original images ranges from 126 to 154 mt (about 413 to 505 feet) per pixel. The images have been re-sized to have an image scale of about 100 mt (330 feet) per pixel. North on Dione is 140 to the left".
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