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Today's image is a lovely color view of the impact crater Sor Juana. The crater interior contains smooth material, probably impact melt, that embays the central peak. The rim is relatively sharp, with well developed terraces. Sor Juana does not have its own rays - the bright ray patches containing chains and clusters of secondary craters that are dotted around the scene originated at Hokusai.
Sor Juana is named for Sor Juana Inés de la Cruz (Sister Joan Agnes of the Cross), a nun and poet who lived from 1651 to 1695 in what is now Mexico. Some authorities consider her body of work to be the most important in North America until the arrival of 19th Century poets such as Dickinson and Whitman.
This image was acquired as a high-resolution targeted color observation. Targeted color observations are images of a small area on Mercury's surface at resolutions higher than the 1-kilometer/pixel 8-color base map. During MESSENGER's one-year primary mission, hundreds of targeted color observations were obtained. During MESSENGER's extended mission, high-resolution targeted color observations are more rare, as the 3-color base map covered Mercury's northern hemisphere with the highest-resolution color images that are possible.
Date acquired: April 07, 2011
Image Mission Elapsed Time (MET): 210677654, 210677650, 210677646
Image ID: 102052, 102051, 102050
Instrument: Wide Angle Camera (WAC) of the Mercury Dual Imaging System (MDIS)
WAC filters: 9, 7, 6 (996, 748, 433 nanometers) in red, green, and blue
Center Latitude: 50.8°
Center Longitude: 333.8° E
Resolution: 224 meters/pixel
Scale: Sor Juana crater is about 94 km (58 mi.) in diameter
Incidence Angle: 50.9°
Emission Angle: 1.4°
Phase Angle: 52.3°
North is up in this image.
Image credit: NASA/Johns Hopkins University Applied Physics Laboratory/Carnegie Institution of Washington
Today's image shows three oblique mosaics of Hokusai, a complex crater in Mercury's northern hemisphere. The top mosaic features a view of Hokusai where north is to the left. The bottom left is a color mosaic that also has north to the left. In the bottom right is mosaic with a high incidence angle where north is now to the right. The high incidence angle emphasizes topography differences because the sun's low angle creates long shadows. Evident in all of these mosaics are Hokusai's smooth impact melt covered floor, central peak, ejecta blanket, and terraced walls.
The top mosaic was acquired as a high-resolution targeted observation. Targeted observations are images of a small area on Mercury's surface at resolutions much higher than the 200-meter/pixel morphology base map. It is not possible to cover all of Mercury's surface at this high resolution, but typically several areas of high scientific interest are imaged in this mode each week.
The bottom left color image was acquired as a targeted high-resolution 11-color image set. Acquiring 11-color targets is a new campaign that began in March 2013 and that utilizes all of the WAC's 11 narrow-band color filters. Because of the large data volume involved, only features of special scientific interest are targeted for imaging in all 11 colors.
The bottom right mosaic was acquired as part of MDIS's high-incidence-angle base map. The high-incidence-angle base map complements the surface morphology base map of MESSENGER's primary mission that was acquired under generally more moderate incidence angles. High incidence angles, achieved when the Sun is near the horizon, result in long shadows that accentuate the small-scale topography of geologic features. The high-incidence-angle base map was acquired with an average resolution of 200 meters/pixel.
Instruments: Wide Angle Camera (WAC) and Narrow Angle Camera (NAC) of the Mercury Dual Imaging System (MDIS)
WAC filters: 9, 7, 6 (996, 748, 433 nanometers) in red, green, and blue for color mosaic
Center Latitude: 57.66°
Center Longitude: 16.58° E
Scale: Hokusai is about 85 km (53 miles) in diameter.
Image credit: NASA/Johns Hopkins University Applied Physics Laboratory/Carnegie Institution of Washington
The top image is a MASCS VIRS color composite of Waters crater (center) in Mercury's mid latitudes. The bottom image is a monochrome MDIS mosaic of the same area. The central blue area corresponds to both Waters and its impact melt flow. The encompassing yellow area likely relates to Waters' ejecta blanket. Blue areas indicate low reflectance, while yellow areas relate to high reflectance and newer material.
The VIRS composite shows hundreds of individual footprints tracks (minimum 100-200 m across and 3-4 km long) taken from different directions and altitudes. In locations where multiple footprints cover the same area, the footprint with the best illumination for mineralogical interpretation (usually the lowest incidence angle where shadows are minimized) is used for making the map. In the MDIS mosaic, some brightness variations are due to tiling of images taken at different illuminations.
Date Created: July 7, 2014
Instruments: Visible and Infrared Spectrograph (VIRS) of the Mercury Atmosphere and Surface Composition Spectrometer (MASCS) and Mercury Dual Imaging System (MDIS)
VIRS Color Composite Wavelengths: 575 nm as red, 415 nm/750 nm as green, 310 nm/390 nm as blue
Center Latitude: -9.1°
Center Longitude: 254.6° E
Resolution: 0.5 km/pixel
Scale: Waters crater (center) is about 15 km (9.3 mi.) in diameter.
Image credit: NASA/Johns Hopkins University Applied Physics Laboratory/Carnegie Institution of Washington
This high-resolution image reveals a few melt ponds, which appear smoother than the surrounding terrain. These melt ponds were deposited as ejecta from this crater, which lies off to the north (top) of this image.
This image was acquired as a high-resolution targeted observation. Targeted observations are images of a small area on Mercury's surface at resolutions much higher than the 200-meter/pixel morphology base map. It is not possible to cover all of Mercury's surface at this high resolution, but typically several areas of high scientific interest are imaged in this mode each week.
Date acquired: March 10, 2014
Image Mission Elapsed Time (MET): 36770132
Image ID: 5908036
Instrument: Narrow Angle Camera (NAC) of the Mercury Dual Imaging System (MDIS)
Center Latitude: 63.77°
Center Longitude: 254.7° E
Resolution: 12 meters/pixel
Scale: The elliptical melt pond is approximately 1 km (0.6 mi.) in length.
Incidence Angle: 72.5°
Emission Angle: 6.3°
Phase Angle: 78.9°
Image credit: NASA/Johns Hopkins University Applied Physics Laboratory/Carnegie Institution of Washington
Ever since MESSENGER entered orbit about Mercury in 2011, the dark impact melt flow of Waters crater has been a feature of interest. Targeted color imaging showed the distinctive blue color of the impact melt flow, inspiring the crater to be named for blues legend Muddy Waters in 2012. In 2013, this high-resolution image was acquired, revealing stunning new details of the impact melt flow beyond those visible previously.
This image was acquired as a targeted set of stereo images. Targeted stereo observations are acquired at resolutions much higher than that of the 200-meter/pixel stereo base map. These targets acquired with the NAC enable the detailed topography of Mercury's surface to be determined for a local area of interest.
Date acquired: September 16, 2013
Image Mission Elapsed Time (MET): 21673915
Image ID: 4834878
Instrument: Narrow Angle Camera (NAC) of the Mercury Dual Imaging System (MDIS)
Center Latitude: -9.00°
Center Longitude: 254.7° E
Resolution: 56 meters/pixel
Scale: Waters crater is 15 kilometers (9 miles) in diameter
Incidence Angle: 44.0°
Emission Angle: 44.8°
Phase Angle: 85.5°
Photo credit: NASA/Johns Hopkins University Applied Physics Laboratory/Carnegie Institution of Washington
Viewing a section of the southern crater in this pair, here we see the jumbled and cracked material on the crater's floor and smooth regions buried by impact melt. Little rock-bergs, tens to hundreds of meters across, dot the floor and are surrounded by a frozen sea of once-molten rock. The Sun is shining from the right.
This image was acquired as a high-resolution targeted observation. Targeted observations are images of a small area on Mercury's surface at resolutions much higher than the 200-meter/pixel morphology base map. It is not possible to cover all of Mercury's surface at this high resolution, but typically several areas of high scientific interest are imaged in this mode each week.
Date acquired: March 10, 2014
Image Mission Elapsed Time (MET): 36770146
Image ID: 5908043
Instrument: Narrow Angle Camera (NAC) of the Mercury Dual Imaging System (MDIS)
Center Latitude: 64.86°
Center Longitude: 255.3° E
Resolution: 12 meters/pixel
Scale: This scene is approximately 6 km (4 miles) across
Incidence Angle: 73.0°
Emission Angle: 5.8°
Phase Angle: 78.9°
Photo credit: NASA/Johns Hopkins University Applied Physics Laboratory/Carnegie Institution of Washington
The name Kuniyoshi was recently adopted by the International Astronomical Union for the 26.5 km diameter crater near the center of today's image. Utagawa Kuniyoshi was a Japanese painter and printmaker (1798-1861). The subjects of his artwork included landscapes, Kabuki scenes, cats, samurai heroes, and the mythical and supernatural. Kuniyoshi crater is morphologically fresh, with a sharp rim, steep central peak, and impact melt ponds on the floor and near-rim ejecta. To the west of Kuniyoshi is a famous Mercurian lobate scarp, Discovery Rupes.
This image was acquired as part of MDIS's high-resolution surface morphology base map. The surface morphology base map covers more than 99% of Mercury's surface with an average resolution of 200 meters/pixel. Images acquired for the surface morphology base map typically are obtained at off-vertical Sun angles (i.e., high incidence angles) and have visible shadows so as to reveal clearly the topographic form of geologic features.
Date acquired: February 25, 2012
Image Mission Elapsed Time (MET): 238701357
Image ID: 1441474
Instrument: Narrow Angle Camera (NAC) of the Mercury Dual Imaging System (MDIS)
Center Latitude: -57.65°
Center Longitude: 321.8° E
Resolution: 173 meters/pixel
Scale: The edges of the image are about 170 km (105 mi.) long.
Incidence Angle: 65.0°
Emission Angle: 0.7°
Phase Angle: 65.2°
Photo credit: NASA/Johns Hopkins University Applied Physics Laboratory/Carnegie Institution of Washington
On March 5 we saw an area to the west of Caloris. Today we travel to the east of the basin, another area that is thought to be related to ejecta from the Caloris basin impact event. The knobs and unusual corrugated texture are part of Odin Planitia and may have formed from ejecta and impact melt. Schiaparelli Dorsum, nearly aligned with the terminator (the division between the dayside and night side of the planet), cuts across the scene from top to bottom.
This image was acquired as part of MDIS's high-incidence-angle base map. The high-incidence-angle base map complements the surface morphology base map of MESSENGER's primary mission that was acquired under generally more moderate incidence angles. High incidence angles, achieved when the Sun is near the horizon, result in long shadows that accentuate the small-scale topography of geologic features. The high-incidence-angle base map was acquired with an average resolution of 200 meters/pixel.
Date acquired: July 07, 2012
Image Mission Elapsed Time (MET): 250134169
Image ID: 2154159
Instrument: Wide Angle Camera (WAC) of the Mercury Dual Imaging System (MDIS)
WAC filter: 7 (748 nanometers)
Center Latitude: 24.83°
Center Longitude: 195.2° E
Resolution: 228 meters/pixel
Scale: This scene is approximately 400 km (250 miles) across
Incidence Angle: 88.8°
Emission Angle: 53.2°
Phase Angle: 142.0°
Photo credit: NASA/Johns Hopkins University Applied Physics Laboratory/Carnegie Institution of Washington
The beautiful Abedin crater is featured in today's image. The crater's sunlit wall meets the crater floor, which occupies the left side of the scene. The floor is largely covered with rock that was melted by the Abdedin impact, ponded on the crater floor, and has now solidified, cracking as it cooled.
This image was acquired as a high-resolution targeted observation. Targeted observations are images of a small area on Mercury's surface at resolutions much higher than the 200-meter/pixel morphology base map. It is not possible to cover all of Mercury's surface at this high
Date acquired: September 23, 2013
Image Mission Elapsed Time (MET): 22252071
Image ID: 4875876
Instrument: Narrow Angle Camera (NAC) of the Mercury Dual Imaging System (MDIS)
Center Latitude: 62.28°
Center Longitude: 352.0° E
Resolution: 16 meters/pixel
Scale: Abedin crater is 116 km (72 miles) in diameter
Incidence Angle: 83.6°
Emission Angle: 22.1°
Phase Angle: 105.8°
Photo credit: NASA/Johns Hopkins University Applied Physics Laboratory/Carnegie Institution of Washington
This lovely, fresh, complex crater with a crescent-shaped central peak was recently given the name Giambologna by the International Astronomical Union. The Dutch sculptor Jean Boulogne Giambologna (1529-1608) is most famous for his bronze statues of the god Mercury. The inset photograph shows one that resides in the Museo Nazionale del Bargello, Florence, Italy. Giambologna crater is distinctive for its wide, terraced western wall and the very smooth impact melt pond that covers the eastern floor. The wall terracing probably resulted from extensive collapse that happened because Giambologna formed on a slope -- the wall of an older, larger crater.
This image was acquired as part of MDIS's high-resolution stereo imaging campaign. Images from the stereo imaging campaign are used in combination with the surface morphology base map or the albedo base map to create high-resolution stereo views of Mercury's surface, with an average resolution of 200 meters/pixel. Viewing the surface under the same Sun illumination conditions but from two or more viewing angles enables information about the small-scale topography of Mercury's surface to be obtained.
Date acquired: October 15, 2011
Image Mission Elapsed Time (MET): 227171471
Image ID: 888364
Instrument: Narrow Angle Camera (NAC) of the Mercury Dual Imaging System (MDIS)
Center Latitude: -42.86°
Center Longitude: 236.7° E
Resolution: 202 meters/pixel
Scale: Giambologna crater is about 67 km (42 mi.) in diameter; Giambologna's Mercury is 180 cm (71 in.) tall
Incidence Angle: 65.8°
Emission Angle: 23.9°
Phase Angle: 67.8°
Image credit: NASA/Johns Hopkins University Applied Physics Laboratory/Carnegie Institution of Washington
The left side of today's image is dominated by an unnamed 75-km-diameter impact crater. The crater has several interesting features. Its western wall is quite broad, with extensive terracing and landslide scarps. The floor of the crater is flat, having been filled by volcanic plains or impact melt. The small central peaks, parts of the floor, and spots along the eastern rim are dotted with high-reflectance hollows. Finally, as outlined in the inset, the ejecta to the north and east of the rim appears to have flowed along the ground, and formed a terminal scarp. A recent paper by Beary Xiao and Goro Komatsu discusses this and other Mercurian craters that have flow-like ejecta, and makes comparisons with similar landforms on the Moon and Mars.
Z. Xiao and G. Komatsu (2013), Impact craters with ejecta flows and central pits on Mercury, Planetary and Space Science, vol. 82-83, pp. 62-78.
This image was acquired as part of MDIS's high-resolution stereo imaging campaign. Images from the stereo imaging campaign are used in combination with the surface morphology base map or the albedo base map to create high-resolution stereo views of Mercury's surface, with an average resolution of 200 meters/pixel. Viewing the surface under the same Sun illumination conditions but from two or more viewing angles enables information about the small-scale topography of Mercury's surface to be obtained.
Date acquired: November 03, 2011
Image Mission Elapsed Time (MET): 228803487
Image ID: 966206
Instrument: Wide Angle Camera (WAC) of the Mercury Dual Imaging System (MDIS)
WAC filter: 7 (748 nanometers)
Center Latitude: 13.45°
Center Longitude: 298.0° E
Resolution: 182 meters/pixel
Scale: The scene is about 190 km (118 mi.) across
Incidence Angle: 68.6°
Emission Angle: 15.5°
Phase Angle: 55.3°
North is up in this image.
Image credit: NASA/Johns Hopkins University Applied Physics Laboratory/Carnegie Institution of Washington
Here we get a closer look at the fresh, bright-rayed crater Mena. Solidified impact melt forms a smooth pond on the western side of the crater floor. This asymmetry is due to the fact that Mena formed on the sloping rim of an older crater, as seen in this wider view.
This image was acquired as a targeted set of stereo images. Targeted stereo observations are acquired at resolutions much higher than that of the 200-meter/pixel stereo base map. These targets acquired with the NAC enable the detailed topography of Mercury's surface to be determined for a local area of interest.
Date acquired: November 13, 2013
Image Mission Elapsed Time (MET): 26657614
Image ID: 5189176
Instrument: Narrow Angle Camera (NAC) of the Mercury Dual Imaging System (MDIS)
Center Latitude: -0.24°
Center Longitude: 235.3° E
Resolution: 37 meters/pixel
Scale: Mena crater has a diameter of 15 km (9 miles)
Incidence Angle: 54.7°
Emission Angle: 23.4°
Phase Angle: 71.0°
Photo credit: NASA/Johns Hopkins University Applied Physics Laboratory/Carnegie Institution of Washington
In the center of this image is a high-reflectance area that seems to be confined to a region of lower elevation that is bounded by linear scarp (cliff) segments. Such diffuse bright areas are sometimes related to the deposition of small secondary craters and ray segments by a relatively recent impact crater, but looking at regional images (for example, using QuickMap), there are no rayed craters in the immediate vicinity (though Han Kan might be a candidate). Therefore, a compositional difference may account for the difference in the albedo (brightness) of the material in the low-lying area. Are the scarps tectonic in nature (the result of vertical movement along faults), or were they formed by secondary crater chains? Also of interest in the scene are hollows on the central peak of the crater at the upper left, and the smooth impact melt on the floor of the terrace-walled crater just below center. Scientists will be at work for many years to solve the puzzle of Mercury's complicated geological history!
This image was acquired as part of the NAC ride-along imaging campaign. When data volume is available and MDIS is not acquiring images for its other campaigns, high-resolution NAC images are obtained of the surface. These images are designed not to interfere with other instrument observations but take full advantage of periods during the mission when extra data volume is available.
Date acquired: May 19, 2012
Image Mission Elapsed Time (MET): 245904903
Image ID: 1853014
Instrument: Narrow Angle Camera (NAC) of the Mercury Dual Imaging System (MDIS)
Center Latitude: -47.3°
Center Longitude: 177.3° E
Resolution: 179 meters/pixel
Scale: The scene is about 184 km (114 mi.) across
Incidence Angle: 47.7°
Emission Angle: 24.2°
Phase Angle: 71.9°
Photo credit: NASA/Johns Hopkins University Applied Physics Laboratory/Carnegie Institution of Washington
The Warhol crater hosts one of the best collections of hollows found on Mercury's surface. The crater's central peak is surrounded by a network of small hollows and a smooth floor formed from impact melt. The hollows seen in the Warhol crater have high albedos, making them easy to see.
This image was acquired as a high-resolution targeted observation. Targeted observations are images of a small area on Mercury's surface at resolutions much higher than the 200-meter/pixel morphology base map. It is not possible to cover all of Mercury's surface at this high resolution, but typically several areas of high scientific interest are imaged in this mode each week.
Date acquired: September 23, 2013
Image Mission Elapsed Time (MET): 22253846
Image ID: 4875892
Instrument: Narrow Angle Camera (NAC) of the Mercury Dual Imaging System (MDIS)
Center Latitude: -2.55°
Center Longitude: 354.1° E
Resolution: 79 meters/pixel
Scale: Warhol is about 91 km (~57 mi.) in diameter
Incidence Angle: 78.5°
Emission Angle: 35.1°
Phase Angle: 113.6°
Photo credit: NASA/Johns Hopkins University Applied Physics Laboratory/Carnegie Institution of Washington
Named for the Roman poet Gaius Valerius Catullus, this impact crater, 100 km (62 mi.) in diameter, has a smoothly textured floor like that seen elsewhere on Mercury. The western portion of the floor (right) abuts against the inner, terraced wall of the crater (middle), which is bordered by the surrounding, older terrain (left). Scientists know of two ways to render the floor of a crater smooth: impact melt or volcanism. It can be difficult to differentiate the two processes, however, and so the nature of the smooth material within Catullus remains unknown. However, in a larger view a depression can be seen in the center of Catullus that may be volcanic in nature -- and so too might the floor of the crater itself.
This image was acquired as a high-resolution targeted observation. Targeted observations are images of a small area on Mercury's surface at resolutions much higher than the 200-meter/pixel morphology base map. It is not possible to cover all of Mercury's surface at this high resolution, but typically several areas of high scientific interest are imaged in this mode each week.
Date acquired: August 8, 2013
Image Mission Elapsed Time (MET): 18306428
Image ID: 4595268
Instrument: Narrow Angle Camera (NAC) of the Mercury Dual Imaging System (MDIS)
Center Latitude: 21.98°
Center Longitude: 293.43° E
Resolution: 39 meters/pixel
Scale: The field of view in this image is approx. 40 km (25 mi.) across
Incidence Angle: 68.1°
Emission Angle: 3.5°
Phase Angle: 71.6°
North is down in this image.
Photo credit: NASA/Johns Hopkins University Applied Physics Laboratory/Carnegie Institution of Washington
This close up of Degas crater shows off its grand central peaks, which are made up of sub-surface material uplifted by the impact. Over time, material from the tops of the central peaks has slid downslope, exposing fresh material that appears bright in this image. The long cracks appearing around the central peaks were likely formed as the impact melt in the bottom of the crater cooled.
This image was acquired as a high-resolution targeted observation. Targeted observations are images of a small area on Mercury's surface at resolutions much higher than the 200-meter/pixel morphology base map. It is not possible to cover all of Mercury's surface at this high resolution, but typically several areas of high scientific interest are imaged in this mode each week.
Date acquired: September 17, 2013
Image Mission Elapsed Time (MET): 21761231
Image ID: 4841024
Instrument: Narrow Angle Camera (NAC) of the Mercury Dual Imaging System (MDIS)
Center Latitude: 36.99°
Center Longitude: 232.8° E
Resolution: 18 meters/pixel
Scale: Degas is 55 km (approximately 34 mi.) in diameter.
Incidence Angle: 67.9°
Emission Angle: 1.6°
Phase Angle: 66.2°
Orientation: North is towards the bottom of the image.
Photo credit: NASA/Johns Hopkins University Applied Physics Laboratory/Carnegie Institution of Washington
This dramatic image features Hokusai in the foreground, famous for its extensive set of rays, some of which extend for over a thousand kilometers across Mercury's surface. The extensive, bright rays indicate that Hokusai is one of the youngest large craters on Mercury. Check out previously featured images to see high-resolution details of its central peaks, rim and ejecta blanket, and impact melt on its floor.
This image was acquired as part of MDIS's high-incidence-angle base map. The high-incidence-angle base map complements the surface morphology base map of MESSENGER's primary mission that was acquired under generally more moderate incidence angles. High incidence angles, achieved when the Sun is near the horizon, result in long shadows that accentuate the small-scale topography of geologic features. The high-incidence-angle base map was acquired with an average resolution of 200 meters/pixel.
Date acquired: September 17, 2013
Image Mission Elapsed Time (MET): 21704875
Image ID: 4836938
Instrument: Wide Angle Camera (WAC) of the Mercury Dual Imaging System (MDIS)
WAC filter: 7 (748 nanometers)
Center Latitude: 58.2.°
Center Longitude: 14.2.° E
Scale: Hokusai has a diameter of 114 km (71 miles)
Orientation: This image is oriented such that north is roughly to the right.
Photo credit: NASA/Johns Hopkins University Applied Physics Laboratory/Carnegie Institution of Washington
The crater Erte, the pseudonym of Romain de Tirtoff was a Russian-born French artist and designer who passed away in 1990. The crater that bears his name is a complex crater that is 48.5 km in diameter (30 miles). Here the flat floor of the crater meets the crater rim and the surrounding ejecta blanket.
Date acquired: April 20, 2013
Image Mission Elapsed Time (MET): 8771355
Image ID: 3917367
Instrument: Narrow Angle Camera (NAC) of the Mercury Dual Imaging System (MDIS)
Center Latitude: 28.14°
Center Longitude: 242.8° E
Resolution: 29 meters/pixel
Scale: The image is 44 km (27 miles) across.
Incidence Angle: 40.8°
Emission Angle: 20.4°
Phase Angle: 61.3°
Photo credit: NASA/Johns Hopkins University Applied Physics Laboratory/Carnegie Institution of Washington
This WAC (Wide Angle Camera) image shows a large portion of the planet, known as a limb image. Prominent in this image is Waters crater in the top left corner, distinctive because of its bright rays and dark impact melt flow. Also identifiable in this picture are Beethoven basin, as well as the Bello crater, Rumi crater, Philoxenus crater, and partly visible: Palmer Rupes.
Date acquired: April 14, 2011
Image Mission Elapsed Time (MET): 211284337
Image ID: 130687
Instrument: Wide Angle Camera (WAC) of the Mercury Dual Imaging System (MDIS)
WAC filter: 7 (748 nanometers)
Center Latitude: -21.12°
Center Longitude: 249.8° E
Resolution: 884 meters/pixel
Scale: Mercury's diameter is 4880 kilometers (3030 miles).
Incidence Angle: 69.6°
Emission Angle: 63.7°
Phase Angle: 28.0°
Photo credit: NASA/Johns Hopkins University Applied Physics Laboratory/Carnegie Institution of Washington
This image focuses on the central peaks and impact melt of Hokusai crater. The contrast between the illuminated sides of these peaks and their shadows make this a striking image. It is interesting to note that the smooth floor surrounding the mountains was formed from cooling impact melt generated from the heat and energy of the original impact. The crater's name honors the Japanese painter and printmaker, Katsushika Hokusai (1760-1849) who possessed a slight obsession with the famous volcano Mt. Fuji. Hokusai's most well known work is "Mount Fuji Seen Below a Wave at Kanagawa."
Date acquired: July 29, 2011
Image Mission Elapsed Time (MET): 220460258
Image ID: 566860
Instrument: Narrow Angle Camera (NAC) of the Mercury Dual Imaging System (MDIS)
Center Latitude: 58.03°
Center Longitude: 16.52° E
Resolution: 24 meters/pixel
Scale: The image is approximately 28 km wide (17 mi.)
Incidence Angle: 75.4°
Emission Angle: 28.5°
Phase Angle: 104.0°
Photo credit: NASA/Johns Hopkins University Applied Physics Laboratory/Carnegie Institution of Washington
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