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| Piú viste - Mercury |
A-Mercury-Antoniadi Ridge.jpgThe Antoniadi Ridge of Mercury71 visiteMercury Data and Statistics:
Mass (kg) = 3.303e+23
Mass (Earth = 1) = 5,5271e-02
Equatorial radius = 2.439,7 Km
Equatorial radius (Earth = 1) = 3,8252e-01
Mean density (gm/cm^3) = 5,42
Mean distance from the Sun = 57.910.000 Km
Mean distance from the Sun (Earth = 1) = 0,3871
Rotational period (days) = 58,6462
Orbital period (days) = 87,969
Mean orbital velocity = 47,88 Km per second
Tilt of axis = 0,00°
Orbital inclination = 7,004°
Equatorial surface gravity (m/sec^2) = 2,78
Equatorial escape velocity = 4,25 Km per second
Magnitude (Vo) = - 1.9
Mean surface temperature = 179°C
Maximum surface temperature = 427°C
Minimum surface temperature = - 173°C
Atmospheric composition: Helium 42%, Sodium 42%, Oxygen 15%, Other 1%
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B-B-Mercury-PIA02947.jpgIntercrater Plain near Caloris Basin71 visiteCaption NASA originale:"Intercrater Plains and heavily cratered terrain typical of much of Mercury outside the area affected by the formation of the Caloris Basin are shown in this image (FDS 166738) taken during the spacecraft's second encounter with Mercury. Abundant shallow elongate craters and crater chains are present on the intercrater plains.
North is to the top of this image, centered at 56° South, 128° West and measuring about 400 Km across".
Note: The Mariner 10 mission, managed by the Jet Propulsion Laboratory for NASA's Office of Space Science, explored Venus in February 1974 on the way to 3 encounters with Mercury (March and September 1974 and March 1975). The spacecraft took more than 7000 photos of Mercury, Venus, the Earth and the Moon.
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ZZ-Mercury-Scarp-208630.jpgDeep Scarp on Mercury (HR)71 visiteNASA’s MESSENGER Spacecraft captured this image on January 14, 2008, during its closest approach to Mercury. The image reveals a variety of intriguing surface features, including craters as small as 300 yards across.
The image also shows landscapes near Mercury’s Equator on the side of the Planet never before imaged by spacecraft. These highly detailed close-ups enable planetary geologists to study the processes that have shaped Mercury’s surface over the past 4 Billion Years. One of the highest and longest scarps cliffs yet seen on Mercury curves from the top center down across the right side of this image. Great forces in Mercury’s crust have thrust the terrain occupying the left two-thirds of the picture up and over the terrain to the right. An impact crater has subsequently destroyed a small part of the scarp near the top of the image.
This image was taken from a distance of 3600 miles from surface of the Planet and shows a region approximately 100 miles across. MareKromium
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ZP-Mercury-PIA10382.jpgMercury’s Mineralogy71 visiteCaption NASA:"The top plot shows the ground track of observations made by the Visible and Infrared Spectrograph (VIRS) component of the Mercury Atmospheric and Surface Composition Spectrometer (MASCS). The ground track is projected onto a MESSENGER image of the portion of the planet seen in high-resolution by MESSENGER for the first time.
The bottom plot shows the relative spectral reflectance as a function of wavelength at the two locations indicated on the previous graphic. The visible and infrared portions of the spectra are shown for the two nearby areas, one including ejected material from a bright, relatively young crater and the other from surrounding plains. The two spectra have been shifted vertically to match at 850 nm (in the near-infrared).
Differences between the two spectra, most notable in the infrared, are indicative of differences in the mineral abundances in these two regions".MareKromium
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ZZ-Mercury-Craters-Damer_Crater-PIA17812-PCF-LXTT-IPF.jpgThe Walls of Damer (Absolute Natural Colors; credits for the additional process. and color. Dr Paolo C. Fienga/Lunar Explorer Italia/Italian Planetary Foundation)71 visiteThe (relatively) steep Walls of the Impact Crater named Damer are well highlighted in today's APOD. Named after the English sculptor, Anne Seymour Damer (née Conway, she was born in Sevenoaks - UK - on November, 8, 1749 and died in London on May, 28, 1828) earlier this year by the International Astronomical Union (or "IAU", for short), this approx. 60-Km diameter (such as about 37,26 miles) Impact Crater is distinguished by a massive and complex Central Peak that is almost completely covered with Hollows.
Date acquired: November, 13th, 2013
Images Mission Elapsed Time (MET): 26687033
Images ID: 5191249
Instrument: Narrow Angle Camera (NAC) of the Mercury Dual Imaging System (MDIS)
Center Latitude: 36,25° North
Center Longitude: 243,40° East
Solar Incidence Angle: 68,3° (meaning that the Sun, at the time that the picture was taken, was about 21,7° above the imaged Local Mercurian Horizon)
Emission Angle: 3,0°
Sun-Mercury-Messenger (or "Phase") Angle: 65,3°
This frame (which is an Original NASA - MESSENGER Spacecraft's b/w and NON Map-Projected image-mosaic published on the NASA - Planetary Photojournal with the ID n. PIA 17812) has been additionally processed, contrast enhanced, magnified to aid the visibility of the details, Gamma corrected and then colorized in Absolute Natural Colors (such as the colors that a human eye would actually perceive if someone were onboard the NASA - MESSENGER Spacecraft and then looked down, towards the Western Edge of the Mercurian Impact Crater "Damer"), 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 Mercury, each having a different Albedo (---> Reflectivity) and Chemical Composition.MareKromium
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Mercury - Zola Crater from Mariner 10.jpgZola Crater - Mariner 1070 visiteCosa farà Messenger al riguardo? Usando uno strumento chiamato "altimetro laser" determinerà la presenza (o la mancanza) di sostanza liquida nel nucleo esterno del Pianeta, misurando la sua "librazione" (ossìa quella lenta, ma rilevabile, oscillazione di Mercurio attorno al proprio asse di rotazione).
Tale "librazione", qualora esistesse ancora un nucleo esterno liquido (magari anche solo in parte) su cui la componente rocciosa del Pianeta, di fatto, si trovasse a "galleggiare",...
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ZZ-Mercury-Craters-Unnamed_Rayed_Crater-208635.jpgUnnamed Crater with Bright Ejecta Rays (HR)70 visiteDuring its flyby of Mercury on Jan. 14, 2008, NASA’s MESSENGER spacecraft acquired High-Resolution (HR) images of the Planet's surface. This image shows a previously unseen crater with distinctive bright rays of ejected material extending outward from the crater's center.
A chain of craters nearby is also visible. Studying impact craters provides insight into the history and composition of Mercury as well as dynamical processes that occurred throughout our Solar System.
This image is one of 99 taken by the Spacecraft to enable the creation of a large, HR mosaic of the northeast quarter of the Region.MareKromium
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ZZ-Mercury-Craters-Moody_Crater-PIA12044_fig1.jpgMoody Crater70 visiteThe crater identified in this NAC image was named in November 2008 for Ronald Moody, a 20th century Jamaican sculptor and painter (see PIA11762). Moody features a Central Peak or Peak-Ring structure and an Annulus of dark material on its Outer Floor (green arrows). The area inward of the dark ring appears reddish in enhanced color WAC images (see PIA11219), indicating the presence of material different in composition from that of either the dark material or the Crater's immediate surroundings. Dark material has been found associated with other craters on Mercury, including Munch and Poe (see PIA12034). Moody is somewhat unusual for having its dark ring confined to the Crater Floor, rather than forming the crater rim as at Munch and Poe.
Date Acquired: January 14, 2008
Image Mission Elapsed Time (MET): 108829034
Instrument: Narrow Angle Camera (NAC) of the Mercury Dual Imaging System (MDIS)
Resolution: 590 meters/pixel (0,37 miles)
Scale: Moody is about 80 Km (approx. 50 miles) in diameter
Spacecraft Altitude: about 23.100 kilometers (approx. 14.300 miles)MareKromium
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ZZ-Mercury-Volcanic_Features-Vent-PIA15245-PCF-LXTT-IPF.jpgVolcanic Vent on the Edge of Caloris Basin (Absokute Natural Colors; credits for the additional process. and color.: Dr Paolo C. Fienga/Lunar Explorer Italia/Italian Planetary Foundation)70 visiteThis kidney-shaped Surface Depression (which is approximately 23 Km - such as 14,283 miles - across its longest dimension) lies along the Inner Margin of the giant Caloris Basin and it was first imaged during the NASA - MESSENGER Spacecraft's first Fly-By of the innermost Planet in the Solar System, about 2 years ago. The Rimless, non-circular Surface Depression is, in fact, the Vent of a small, explosive Volcano, and it is similar to many other Volcanic Vents that have been discovered on Mercury. The small number of superposed Impact Craters indicates that this Feature is, just in a manner of speaking, relatively "young" as to the surrounding Terrain. Notice, also, the considerable number of bright Hollows that seem to characterize a large portion of the Inner Rim as well as the East-facing Slopes of the small Impact Crater located right outside the Eastern Margin of the Vent, at about 4 o'clock of the Main Feature.
Note: for another view of this Volcanic Vent and its extremely interesting surroundings (seen on a larger scale), please refer to the APOD of December, 22nd, 2012.
Date acquired: June 7th, 2011
Image Mission Elapsed Time (MET): 215894570
Image ID: 347724
Instrument: Narrow Angle Camera (NAC) of the Mercury Dual Imaging System (MDIS)
Center Latitude: 22,5° North
Center Longitude: 146,1° East
Resolution: 28 meters/pixel
Solar Incidence Angle: 39,6° (meaning that the Sun, at the time that the picture was taken, was about 50,4° above the imaged Local Mercurian Horizon)
Emission Angle: 45,5°
Sun-Mercury-Messenger (or "Phase") Angle: 78,3°
This picture (which has been cropped from an Original NASA - MESSENGER Spacecraft b/w frame published on the NASA - Planetary Photojournal with the ID n. PIA 15245) 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 NASA - MESSENGER Spacecraft and then looked down, towards the Surface of Mercury), 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 Mercury, each having a different Albedo (---> Reflectivity) and Chemical Composition.MareKromium
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Mercury 2.jpgMercury close-up from Mariner 10 (1)69 visiteUn'altro mistero che si spera di risolvere con il Messenger attiene il contenuto dei crateri situati nelle regioni polari di Mercurio (l'ipotesi è che sul fondo di questi crateri vi sia del ghiaccio d'acqua vero e proprio). Impossibile? Diremmo proprio di no: queste zone, infatti, grazie alla particolare configurazione dell'asse di rotazione di Mercurio - il quale è perpendicolare al suo piano orbitale - sono esposte, da e per l'eternità, solo ad un'illuminazione radente.
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ZZ-Mercury-Craters-Munch_Crater_et_al_-PIA12034.jpgMunch, Sander and Poe Crater (Natural Colors; credits: Lunar Explorer Italia)69 visitenessun commentoMareKromium
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B-Mercury-HD-PIA02447.jpgScarps confined to crater floors68 visiteCaption NASA originale:"The scarp in this 35-Km crater (See PIA02433 for the location in a larger view) forms a broad lobe 10 Km wide, whose southern end abuts against and follows closely the irregular contour of the crater wall. These structural relations suggest the scarp is a lava flow front rather than a fault.
This image (FDS 27471) was taken by Mariner 10 during its first encounter with Mercury".
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