| Piú votate - Mars through Mars Express (ESA - Original Raw Frames & Orbital Panoramas) |
Aeolian_Features-Yardangs-Eumenides_Dorsum-ESA-ME-424-20081105-5114-6-co-01-H1-PCF-LXTT-IPF.jpgFeatures of Eumenides Dorsum (Absolute Natural Colors; credits for the additional process. and color.: Dr Paolo C. Fienga - Lunexit Team)95 visiteThis frame, which is a mosaic of several orbital images obtained by the High Resolution Stereo Camera onboard the ESA - Mars Express Orbiter, shows us a number of Surface Features; in particular, and in addition to the presence of Plains, Buttes and just a few ancient and semi-buried Impact Craters, we suggest you to pay some special attention to the unbelievable complex of Sinuous Erosional Surface Striations, known as "Yardangs" (which are the most common Aeolian - meaning "sculpted by Wind" - Features that can be found on the Red Planet), that covers a huge portion of the central part of the picture.
All the abovementioned Surface Features are located in the Eumenides Dorsum Region of Mars, which lies to the West of the Tharsis Volcanic Province and forms part of the Region known as Medusae Fossae, at approx. 2° South Latitude and 206° East Longitude. The images here were taken on the date of December, 26, of the AD 2007; they have a ground resolution of about 13 meters per pixel and cover an area (in total) of about 12.000 square Km.
This frame (which is the Original ESA - Mars Express HRST b/w mosaic n. 424-20081105-5114-6-co-01-H1) has 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 ESA - Mars Express Orbiter and then looked down, towards the Surface of Mars), 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 others, the existence of different Elements present on the Surface of Mars, each having a different Albedo (---> Reflectivity) and Chemical Composition.MareKromium
(3 voti)
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Aeolian_features-Yardangs-2-s_015_050504_0143_4_3d_01_Yardangs_FAZ-PCF-LXTT.jpgWind-Lanes (Absolute Natural Colors; credits for the additional process. and color.: Dr Paolo C. Fienga - Lunexit Team)212 visiteCaption ESA originale:"Loose sand fragments were transported by wind, and impacted on the Bedrock, slowly removing parts of the Surface, like a sand-blaster. If the winds blow in the same direction for a long enough period, ‘Wind-Lanes’, as shown in the picture, can occur. On Earth, the remnants of these features which have not been eroded away are called ‘Yardangs’. Where the Surface consists of more resistant material, the force of the wind may not be strong enough to cause this sand-blasting. This might be the reason for the three flat regions (the first in the foreground on the left, and the other two on the top right), which measure about 17 by 9 Km".MareKromium
(3 voti)
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A-h0061_0000_re2-00.jpgFrame h0061_0000_re2 - South Polar Vision (Absolute Natural Colors; credits for the additional process. and color.: Dr Paolo C. Fienga - Lunexit Team)237 visitenessun commentoMareKromium
(3 voti)
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Hellas_Planitia-H0572_0000_ND2_H-PCF-LXTT.jpgFrame H0572_0000_ND2: Hellas Planitia Region203 visiteCaption ESA:"The HRSC on board ESA's Mars Express Spacecraft obtained this image on July, 1st, 2004 during orbit 572 with a ground resolution of approx. 45,1 mt per pixel.
The scene shows a portion of Hellas Planitia, a Region which is about 234 Km wide in the North, 345 Km in the South, about 898 Km in length, and centred at approx. 89° East Long. and 29° South Lat.
This image represents an area on the Northern Eastern Rim of Hellas Planitia, also known as the Hellas Impact Basin in Mars's Southern Hemispere. The Basin is thought to have formed around 3900 Million Years ago in a single massive impact".MareKromium
(3 voti)
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Hesperia_Planum-224co01_H-PCF-LXTT.jpgHuge Massif in Hesperia Planum233 visiteCaption ESA:"The HRSC on ESA's Mars Express obtained this image on June, 13th, 2004, during orbit 506 with a ground resolution of approx. 37,6 mt per pixel.
This view shows a portion of the Hesperia Planum Region, containing the Massif, and located at approx. 30,3° South Lat. and 97,8° East Long.".MareKromium
(3 voti)
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CR-h0500_0000_nd3-00-PCF-LXTT.jpgFrame h0500_0000_nd3-00 - Yardangs and Crater Cluster (Natural Colors; credits for the additional process. and color.: Dr Paolo C. Fienga - Lunexit Team)196 visitenessun commentoMareKromium
(3 voti)
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CR-h0550_0000_nd3-01-PCF-LXTT.jpgFrame h0550_0000_nd3-01 - Rayed Crater and Collapse Features (Natural Colors; credits for the additional process. and color.: Dr Paolo C. Fienga - Lunexit Team)219 visitenessun commentoMareKromium
(3 voti)
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Tiu_Valles-ESA-PCF-LXTT.jpgTiu Valles (Natural Colors; credits: Dr Paolo C. Fienga - Lunexit Team)70 visiteThis image taken by the High Resolution Stereo Camera (HRSC) on board Mars Express shows the mouth of the Tiu Valles Channel System on the Red Planet. The picture was taken in orbit 3103 on 10 June 2006 with a ground resolution of approx. 16 mt/pixel. Visible in the lower part of the image are remnants of a once 'Streamlined' Island. The upper part of the scene covers the mouth of the Tiu Valles nearly in its entire width, approx. 55 Km.
Its winding, meandering Ridges, bound by depressions are eye-catching. The processes that formed these odd structures are still unknown. Possibly, during flooding events, water or water-rich surface layers came in contact with lava from the surrounding areas, which then might have led to the formation of these mysterious ridges.
The Region is located at approx. 27° North Lat. and 330° East Long. The Sun illuminates the scene from the North West, the lower left-hand side in the image. MareKromium
(3 voti)
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Phobos-400-455-20091201.jpgBig Brother and Little Brother56 visitePhobos and Deimos RAW (left panel) and processed images (right panel).
In a first, ESA’s Mars Express Orbiter imaged the Martian Moons Phobos and Deimos together on November, 5th, 2009.
Apart from their ‘wow’ factor, these unique images will help the HRSC team validate and refine existing orbit models of the two moons.
The images were acquired with the Super Resolution Channel (SRC) of the High Resolution Stereo Camera (HRSC). The camera took 130 images of the moons on November 5th at 09:14 CET in a span of 1,5 minutes at intervals of 1", speeding up to 0,5" intervals toward the end. The image resolution is 110 m/pixel for Phobos and 240 m/pixel for Deimos — Deimos was more than twice as far from the camera.
The Super Resolution Channel of the HRSC uses an additional lens, which has a very narrow field of view of just 0,5°, providing four times the magnification than otherwise providing four times the resolution of the HRSC colour stereo channel.
Phobos, the larger of the two moons, orbits closer to the Red Planet, circling it every 7 hours and 39 minutes. It travels faster relative to Mars than the Moon relative to Earth.
Phobos was about 11.800 Km from Mars Express when the images were taken. Deimos, instead, was about 26.200 Km away.MareKromium
(3 voti)
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SouthPole-MG_SP_Fig02a_H.jpgThe South Pole of Mars (natural colors; credits: Lunexit)54 visiteCaption ESA:"This is a mosaic of images taken by the Mars Express’s Visible and Infrared Mineralogical Mapping Spectrometer, OMEGA.
It shows the Residual South Polar Cap at the end of Northern Winter on the Red Planet. The cap appears clearly asymmetric, its centre being displaced by 3° from the Geographic Pole".MareKromium
(3 voti)
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Phobos-404-20080729-5181-6-an-01-Phobos-Flyby_2_H1.jpgPhobos in 3D (red-cyan anaglyph)54 visiteCaption ESA:"On July 23, 2008, the High Resolution Stereo Camera on board ESA’s Mars Express took the highest-resolution full-disc image yet of the surface of the moon Phobos.
This image data was acquired from a distance of about 97 Km with a spatial resolution of about 3,7 m/pixel".MareKromium
(3 voti)
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Echus_Chasma-398-260508-2204-6-co-01-H2.jpgHigh Cliffs Surrounding Echus Chasma on Mars58 visiteWhat created this great cliff on Mars? Did giant waterfalls once plummet through its grooves? With a four-kilometer drop, this high cliff surrounding Echus Chasma, near an impressive impact crater, was carved by either water or lava. A leading hypothesis is that Echus Chasma, at 100-Km long and 10-Km wide, was once one of the largest water sources on Mars. If true, water once held in Echus Chasma likely ran over the Martian Surface to carve the impressive Kasei Valles, which extends over 3000 Km to the North. Even if initially carved by water, lava appears to have later flowed in the valley, leaving an extraordinarily smooth floor. Echus Chasma lies north of tremendous Valles Marineris, the largest canyon in the Solar System. The above image was taken by the robotic Mars Express spacecraft currently orbiting Mars.
Nota Lunexit: checchè ne dica la NASA, questo frame NON E' una fotografia.MareKromium
(3 voti)
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