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009-1-Ceres-PIA19884-PCF-LXTT-IPF-1.jpgWhite Unnamed Crater on 1-Ceres (Absolute Natural Colors; credits for the additional process. and color.: Dr Paolo C. Fienga/Lunar Explorer Italia/Italian Planetary Foundation)59 visiteToday's APOD is an Extra Detail Magnification (or "EDM", for short) of yesterday's Contextual (or "CTX", for short) Frame, taken by the NASA - Dawn Spacecraft that shows us a small White Crater (---> also informally known as "White Spot") that is located in the Northern Hemisphere of the Dwarf Planet named 1-Ceres.
Now, we ask you one (extremely complicated, in fact) question that you, however, should try to answer: why, on 1-Ceres, the huge and deep Impact Craters do not show "White Material" inside them, while, on the other hand, the small and shallow ones (Impact Craters) do? Probably because, but we, as IPF, cannot be sure of this (just like everyone else), the White Material, in the end, does not belong to/comes from the Sub-Surface of 1-Ceres (as we thought, at the beginning), but it belongs to/comes from the Impactors. And you, what do you think?...If you want to share your opinion, please, write us at alphacentauri@intercom.it
The picture was taken from an altitude of approx. 915 miles (such as about 1472,5461 Km) from the Surface, with a resolution of roughly 450 feet (such as about 137,16 meters) per pixel, was taken on August 21, 2015.
This image (which is a crop taken from an Original NASA - Dawn Spacecraft's b/w and NON Map-Projected frame published on the NASA - Planetary Photojournal with the ID n. PIA 19884 - Dawn HAMO Image 8) has been additionally processed, extra-magnified to aid the visibility of the details, contrast enhanced and sharpened, Gamma corrected and then colorized (according to an educated guess carried out by Dr Paolo C. Fienga-LXTT-IPF) in Absolute Natural Colors (such as the colors that a normal human eye would actually perceive if someone were onboard the NASA - Dawn Spacecraft and then looked ahead, towards the Surface of 1-Ceres), by using an original technique created - and, in time, dramatically improved - by the Lunar Explorer Italia Team.MareKromium
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010-1-Ceres-PIA19898-PCF-LXTT-IPF.jpgUnnamed Crater on the Terminator of 1-Ceres (Absolute Natural Colors; credits for the additional process. and color.: Dr Paolo C. Fienga/Lunar Explorer Italia/Italian Planetary Foundation)59 visiteThis simply beautiful Contextual (or "CTX", for short) Frame, taken by the NASA - Dawn Spacecraft on August, 26, 2015, shows us, among other interesting things, an Ancient and extremely Complex Unnamed Impact Crater (which seems to be characterized by the presence of an unusually-looking - we would say, as IPF, "columnarly-shaped", maybe? - Central Peak) that is located near the Terminator Line of the Dwarf Planet named 1-Ceres.
If you will pay attention to the frame, you might agree on the fact that the long shadows - which are very well visible all over the picture - make the whole scene - with its deeply complex Surface Details - even more suggestive.
The picture was taken from an altitude of approx. 915 miles (such as about 1472,5461 Km) from the Surface, with a resolution of roughly 450 feet (such as about 137,16 meters) per pixel, was taken on August 21, 2015.
This image (which is an Original NASA - Dawn Spacecraft's b/w and NON Map-Projected frame published on the NASA - Planetary Photojournal with the ID n. PIA 19898 - Dawn HAMO Image 20) has been additionally processed, extra-magnified to aid the visibility of the details, contrast enhanced and sharpened, Gamma corrected and then colorized (according to an educated guess carried out by Dr Paolo C. Fienga-LXTT-IPF) in Absolute Natural Colors (such as the colors that a normal human eye would actually perceive if someone were onboard the NASA - Dawn Spacecraft and then looked ahead, towards the Surface of 1-Ceres), by using an original technique created - and, in time, dramatically improved - by the Lunar Explorer Italia Team.MareKromium
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APOLLO 15 AS 15-9874.jpgAS 15-9874 - Dawes Crater53 visiteThis is a near vertical view of the crater Dawes, 18 Km in diameter. Morphologically it is typical of many lunar craters in the 15- to 20-Km size range. It lacks terraced walls and distinct central peaks but has an extremely rough floor. Small terracelike structures on the crater floor (upper left, lower right) occur where the wall is bowed outward and probably represent slump deposits where portions of the crater wall have collapsed into the crater. Local stratigraphy is revealed in the walls of the crater, and material of different albedo is seen streaming down into the crater from various levels. The dark layer clearly visible in the upper part of the crater wall represents the thin mare deposits in this part of Northern Mare Tranquillitatis. The lighter gray material below it is a combination of underlying submare material and talus from units higher on the crater wall. The highest unit (white and gray) probably represents the ejecta blanket and may consist primarily of lighter lunar crustal material excavated from beneath the mare.
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APOLLO 15-0326.jpgAPOLLO 15-0326 - Aristarchus61 visiteAristarchus is a large crater on the edge of a plateau within Northern Oceanus Procellarum. In this scene the crater is viewed obliquely from the North. One of the brightest and youngest craters of its size on the Near-Side of the Moon, Aristarchus is believed to be younger even than Copernicus. The general appearance of Aristarchus and of parts of the plateau around it led Alfred Worden, the Apollo 15 CMP, to describe this part of the Moon as "... probably the most volcanic area that I've seen anywhere on the surface". For many years before the Apollo Missions, Earth-based viewers had reported telescopic sightings of TLP's centered on Aristarchus. These brief, subtle changes in color or in sharpness of appearance have been suggested as evidence for volcanic activity or the venting of gases from the lunar interior. The sightings are controversial, but Aristarchus remains a center of interest.
About 39 Km in diameter, Aristarchus is on the borderline between medium-sized and large- sized craters. We have included it among the large craters because its welldeveloped concentric terraces are characteristic of most large craters that have not been too severely degraded. Its terraced walls, as well as its arcuate range of central peaks, are particularly well shown in this view. The walls and parts of the crater floor are extremely rough and cracked, a characteristic feature of other young impact craters of this size range, such as Tycho and Copernicus. The rough deposits in the floor are probably made up largely of shockmelted material formed at the time of the impact. The inner, rougher portions of the rim show a series of channels, lobate flows, and smooth puddlelike deposits that may represent shock-melted material deposited on the crater rim. The outer, smoother portions show the rhomboidal pattern characteristic of crater ejecta blankets.
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APOLLO_11_AS_11-37-5455-PCF-LXTT-IPF.jpgAS 11-37-5455 - Here's the "Flare-like light"! (Frame restored and recalibrated; credits: Dr Paolo C. Fienga/LXTT/IPF) 147 visiteThis is an historical picture taken by the NASA - Apollo 11 Astronaut "Buzz" Aldrin from his own window; it forms part of a five-frames panorama and it shows the Lunar Surface just after landing, with the Lunar Module shadow and the Lunar Horizon.
The "Flare-like Light" that is very well visible on the right (Dx) side of the frame, very close to the Horizon, is one of the many "misteries" that were found during the analysis of the whole Apollo - Moon Collection. Said that, the question is (relatively...) "simple": is this "Flare-like Light" a real - and, perhaps, just "temporary" - Feature of the Lunar Surface (a "flare", for instance, like it was originally speculated by Dr Paolo C. Fienga/LXTT/IPF, and then confirmed by a former Member of the Lunar and Planetary Institute), or is it just one of the very many image-artifacts (---> such as, basically, "defects" of the picture caused by some imperfection in the camera lenses and/or in the film itself) that can also be found in the Apollo - Moon Collection?
Of course we, as IPF, do not have a final answer to this question and, apparently, nobody does (even though a former NASA's Image Technician wrote us saying that the "shining light" was a true Surface Feature and, in his opinion, "...the result of Sunlight that was illuminating a distant - but highly reflective - boulder...". An opinion, this one, that we deeply respect but, honestly speaking, that we also consider extremely unlikely: consider, in fact, that no light whatsoever is visible in that precise spot in the frame that follows this one - such as AS 11 37-5456 -; a frame that was taken only a few seconds after AS 11 37-5455. Now, if this "light" was really just a reflection caused by Sunlight illuminating an highly reflective boulder, it is logical and reasonable to assume that the "reflection" should have still been very well visible over there, even a few seconds (and, maybe, also for a few minutes) after the time when "Buzz" took the first picture of his "Window Panorama". But this - we repeat: reasonable and logical - "circumstance", as a matter of fact, did not happen. The Flare-like Light (or the reflection, if you prefer) vanished very quickly. Why? Of course no answer even to this last question was ever given.
Anyway, the "Flare-like Light" (which may also look like a "Metallic Reflection" in the LPI frame) is there and, in a way, it keeps "asking" us to be recognized and identified, beyond any reasonable doubt, for what that it really was. Maybe, in the Future, we shall know more. Or, maybe (and most likely), the "Flare-like Light" shall remain a Lunar Mistery forever...
This bigger picture (which is an Original NASA - APOLLO 11 Spacecraft color frame published on the NASA - Apollo 11 Lunar Surface Journal with the ID n. AS 11-37-5455) has been additionally processed and then re-colorized in Absolute Natural Colors (such as the colors that a human eye would actually perceive if someone were onboard the NASA - Apollo 11 Lunar Module and then looked outside, towards the Surface and Horizon of the Moon), by using an original technique created - and, in time, dramatically improved - by the Lunar Explorer Italia Team. Different colors, as well as different shades of the same color, mean, among other things, the existence of different Elements (Minerals) present on the Surface of the Moon, each having a different Albedo (---> Reflectivity) and Chemical Composition.
The smaller (inset) picture, is also an Original NASA - APOLLO 11 Spacecraft color frame published by the Lunar and Planetary Institute (LPI) on the Apollo Image Atlas with the ID n. AS 11-37-5455. This second picture HAS NOT been additionally processed nor re-colorized by Lunar Explorer Italia.MareKromium
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A_Pair_of_Small_Pit_Craters_(PSP_009488_1745)-3.jpgCollapse Pit66 visiteThe ability to detect and explore Martian Caves is of intense interest to many disciplines in Planetary Science. Caves may expose entire sets of stratigraphic layers, providing windows into Mars' Geologic and Atmospheric histories.
Cave environments can also protect organic life from extremely harsh conditions on the Martian Surface, and may provide future human explorers with secure habitats. Accordingly, Caves are considered among the most promising locations to find preserved evidence of past or present microbial life.
Furthermore, the challenges associated with Mars Cave exploration may inspire a range new technologies, such as advanced robotics and target-specific landing capabilities.MareKromium
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Albategnius-2.jpgAlbategnius Crater (2)121 visiteAlbategnius (Al-Battani, Muhammad ibn Jabir) (approx. 850-929)
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An Iraqi prince, born in Batan, Mesopotamia (Iraq), who was the leading Astronomer and Mathematician of his time. He drew up improved tables of the Sun and Moon, measured the eccentricity of Earth’s orbit and the inclination of Earth’s Equator to its orbital plane. He was capable of making an extremely accurate measurement of the length of the Earth year - which was also used in the Gregorian reform of the Julian Calendar. His observations at Rakku, made over (probably) a 40-year period, were summarized in his work "Movements of the Stars" (first published in Europe in 1537).
Thanks to his contribution, Johannes Hevelius (1611-1687) was able to theorize and discover the secular variation in the Moon’s motion.
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Amalthea and Io-PIA01626.jpgAmalthea and Io (approx. true colors)131 visiteComposite view of Amalthea and Io at the same scale. The visible part of Amalthea is about 150 Km across. The colors are just approximate. Amalthea is actually much darker than Io, but is displayed at a similar brightness for ease of viewing. The shape of Amalthea is controlled largely by impact cratering and fragmentation. In contrast, Io, like Earth, has gravity sufficient to form it into a slightly ellipsoidal sphere. Amalthea is covered by craters because there are no processes which erode or cover them efficiently. On extremely volcanically active Io, impact craters are covered quickly by lavas and other volcanic materials. Some of the volcanic materials escape from Io and probably contribute to the reddish colors of Amalthea and the other small inner satellites. The Amalthea and Io composites, obtained by the Solid State Imaging (SSI) camera on NASA's Galileo spacecraft on different orbits, were placed side by side for comparison purposes. The Amalthea composite combines data taken with the clear filter of the SSI system during orbit six, with lower resolution color images taken with the green, violet, and 1 micrometer filters during orbit 4. The Io data was obtained on July 2nd, 1998 (orbit 14) using the green, violet, and 1 micrometer filters.
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Anthe-PIA11100.jpgThe "Anthe Arc"65 visiteCaption NASA:"Caption NASA:"Cassini images reveal the existence of a faint "Arc of material" orbiting with Saturn's small moon Anthe.
The moon is moving downward and to the right in this perspective. In this image, most of the visible material in the Arc lies ahead of Anthe (2 Km, or a little more than 1 mile across) in its orbit. However, over time the moon drifts slowly back and forth with respect to the Arc.
The Arc extends over about 20° in Longitude (about 5,5% of Anthe's orbit) and appears to be associated with a gravitational resonance caused by the moon Mimas). Micrometeoroid impacts on Anthe are the likely source of the Arc material.
The orbit of Anthe lies between the larger moons Mimas and Enceladus. Anthe shares this region with two other small moons, Pallene (4 Km, or about 3 miles across) and Methone (3 Km, or approx. 2 miles across).
Methone also possesses an Arc (see PIA11102), while Pallene is known to orbit within a faint, complete ring of its own (see PIA08328).
Cassini imaging scientists believe the process that maintains the Anthe and Methone Arcs is similar to that which maintains the Arc in the G-Ring (see PIA08327). The general brightness of the image (along with the faint horizontal banding pattern) results from the long exposure time of 32" required to capture the extremely faint ring arc and the processing needed to enhance its visibility (which also enhances the digital background noise in the image). The image was digitally processed to remove most of the background noise. The long exposure also produced star trails in the background.
The image was taken in visible light with the Cassini Spacecraft narrow-angle camera on April 4, 2008. The view was acquired at a distance of approx. 1,2 MKM (such as about 746.000 miles) from Anthe and at a Sun-Anthe-Spacecraft Angle of 23°. Image scale is roughly 7 Km (about 4 miles) per pixel".MareKromium
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Anthe-PIA11101.jpgThe "Anthe Arc"54 visiteCaption NASA:"Cassini images reveal the existence of a faint "Arc of material" orbiting with Saturn's small moon Anthe.
The moon is moving downward and to the right in this perspective. In this image, most of the visible material in the Arc lies ahead of Anthe (2 Km, or a little more than 1 mile across) in its orbit. However, over time the moon drifts slowly back and forth with respect to the Arc.
The Arc extends over about 20° in Longitude (about 5,5% of Anthe's orbit) and appears to be associated with a gravitational resonance caused by the moon Mimas). Micrometeoroid impacts on Anthe are the likely source of the Arc material.
The orbit of Anthe lies between the larger moons Mimas and Enceladus. Anthe shares this region with two other small moons, Pallene (4 Km, or about 3 miles across) and Methone (3 Km, or approx. 2 miles across).
Methone also possesses an Arc (see PIA11102), while Pallene is known to orbit within a faint, complete ring of its own (see PIA08328).
Cassini imaging scientists believe the process that maintains the Anthe and Methone Arcs is similar to that which maintains the Arc in the G-Ring (see PIA08327). The general brightness of the image (along with the faint horizontal banding pattern) results from the long exposure time of 32" required to capture the extremely faint ring arc and the processing needed to enhance its visibility (which also enhances the digital background noise in the image). The image was digitally processed to remove most of the background noise. The long exposure also produced star trails in the background.
This view looks toward the un-illuminated side of the Rings from about 3° above the Ring-Plane.
The image was taken in visible light with the Cassini spacecraft narrow-angle camera on July 3, 2008. The view was obtained at a distance of approx. 1,2 MKM (such as about 739.000 miles) from Anthe and at a Sun-Anthe-Spacecraft, or Phase, Angle of 12°. Image scale is roughly 7 Km (about 4 miles) per pixel".MareKromium
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Anthe_Methone-PIA11102.jpgSmall - but VERY bright - Companions: Anthe and Methone55 visiteCaption NASA:"Recent Cassini images show Arcs of Material co-orbiting with the Saturnian moons Anthe and Methone.
Arrows indicate the positions of Anthe, at top left, and Methone, at bottom right. Micrometeoroid impacts on the moons are the likely source of the Arc Material.
Cassini imaging scientists believe the process that maintains the Anthe and Methone arcs is similar to that which maintains the Arc in the G-Ring (see PIA08327). The general brightness of the image (along with the faint horizontal banding pattern) results from the long exposure time of 15" required to capture the extremely faint ring arc and the processing needed to enhance its visibility (which also enhances the digital background noise in the image).
The image was digitally processed to remove most of the background noise. This view looks toward the un-illuminated side of the Rings from about 2° above the Ring-Plane.
The image was taken in visible light with the Cassini Spacecraft narrow-angle camera on Oct. 29, 2007. The view was acquired at a distance of approx. 2,3 MKM (about 1,4 MMs) from Anthe and 2,2 MKM (approx. 1,4 MMs) from Methone.
Image scale is roughly 14 Km (about 9 miles) per pixel on Anthe and 13 Km (approx. 8 miles) on Methone".MareKromium
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BlueSun.jpgBlue Sun53 visiteDa "NASA - Picture of the Day" del giorno 4 Novembre 2009:"Our Sun may look like all soft and fluffy, but it is not. Our Sun is an extremely large ball of bubbling hot gas, mostly Hydrogen gas. The above picture of our Sun was taken last month in a specific red color of light emitted by Hydrogen gas called "Hydrogen-alpha" and then color inverted to appear blue.
In this light, details of the Sun's Chromosphere are particularly visible, highlighting numerous thin tubes of magnetically-confined hot gas known as spicules rising from the Sun like bristles from a shag carpet.
Our Sun glows because it is hot, but it is not on fire. Fire is the rapid acquisition of Oxygen, and there is very little Oxygen on the Sun. The energy source of our Sun is the nuclear fusion of Hydrogen into Helium deep within its core. No Sunspots or large active regions were visible on the Sun this day, although some Solar Prominences are visible around the edges".MareKromium
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