Paramour Rupes

Red-cyan glasses will help you see the impressive heights of Paramour Rupes in this 3D view. Paramour is a large cliff (well over 600 meters high at places!) that formed when one block of crust was thrust forward over another, resulting in a feature known as a lobate scarp. Paramour Rupes is located to the southwest of the Caloris basin, and the small knobs that litter the scene are thought to be blocks of ejecta from the Caloris impact event. For ease of stereo viewing, this anaglyph has been rotated so that north is toward the left.

This image pair 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: June 18, 2014
Image Mission Elapsed Time (MET): 45386688, 45387906
Image ID: 6520353, 6520362
Instrument: Narrow Angle Camera (NAC) of the Mercury Dual Imaging System (MDIS)
Center Latitude: -4.99°
Center Longitude: 146.3°E
Resolution: 110 meters/pixel
Scale: This scene is approximately 110 km (68 miles) across
Incidence Angle: 63.8°
Emission Angle: 37.2°
Phase Angle: 97.7°

Image credit: NASA/Johns Hopkins University Applied Physics Laboratory/Carnegie Institution of Washington

Unnamed Craters

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

Rupes

Today's image features a scarp, or cliff face, which is longer than the 77 km shown in this frame. Scarps form as one block of crust is thrusted forward over another, which can result from the cooling of the planet's interior causing global contraction. On Mercury, scarps are called "rupes," which is Latin for cliff.

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: July 08, 2013
Image Mission Elapsed Time (MET): 15627633
Image ID: 4404792
Instrument: Narrow Angle Camera (NAC) of the Mercury Dual Imaging System (MDIS)
Center Latitude: 20.47°
Center Longitude: 141.0° E
Resolution: 51 meters/pixel
Scale: Image width is about 65 km (40.4 miles)
Incidence Angle: 83.4°
Emission Angle: 38.9°
Phase Angle: 45.4°

Photo credit: NASA/Johns Hopkins University Applied Physics Laboratory/Carnegie Institution of Washington

Enterprise Rupes and Rembrandt Basin

This false-color image is located just at the edge of the Rembrandt Basin. The basin edge crosses the newly named Enterprise Rupes. This is just a small meeting of two titans, as Enterprise extends for ~822 km (510 mi.), and Rembrandt is about 723 km (450 mi) in diameter. The edge of Rembrandt is loosely marked with a pink line, and Enterprise with a yellow line.

Date acquired: August 14, 2011
Image Mission Elapsed Time (MET): 221845855, 221845875, 221845859
Image ID: 632458, 632463, 632459
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: -36.15°
Center Longitude: 75.66° E
Resolution: 576 meters/pixel
Scale: This image is about 640 km (398 mi.) across.
Incidence Angle: 56.7°
Emission Angle: 0.5°
Phase Angle: 56.3°

Photo credit: NASA/Johns Hopkins University Applied Physics Laboratory/Carnegie Institution of Washington

Belgica Rupes

This image highlights the difference between the areas on and below the newly named Belgica Rupes. The arrows show Belgica's location, stretching along most of this image for about 764 km. Notice how some of the smaller, newer craters obscure the scarp line, while the older craters were clearly disrupted by the formation of Belgica Rupes.

The word 'rupes' comes from the latin word for cliff. All rupes on Mercury are named after vehicles of exploration. Belgica was a Belgian ship that explored the south pole of earth in 1898. Belgian Rupes is also very close to the southern pole of Mercury. It's name was approved by the IAU on June 6, 2013 along with 9 other rupes.

Date acquired: August 17, 2011
Image Mission Elapsed Time (MET): 222063126, 222063130, 222063122
Image ID: 642667, 642668, 642666
Instrument: Wide Angle Camera (WAC) of the Mercury Dual Imaging System (MDIS)
WAC filters: 3, 4, 6 (479, 558, 433 nanometers) in red, green, and blue
Center Latitude: -52.80°
Center Longitude: 64.08° E
Resolution: 896 meters/pixel
Scale: Belgica Rupes extends 764 km (475 miles).
Incidence Angle: 63.3°
Emission Angle: 0.4°
Phase Angle: 63.2°

Photo credit: NASA/Johns Hopkins University Applied Physics Laboratory/Carnegie Institution of Washington

Degraded Impact Crater Rim

The rim of an unnamed peak-ring basin cuts across today's featured image. The basin is relatively degraded, but its rim still stands as a cliff over 1 km (0.6 miles) high. The face of this cliff, where downslope is toward the top of the image, is covered by a chain of secondary craters, whose formation on this steep slope led to somewhat asymmetrical crater shapes. It's hard to say which crater these secondaries originated from - the region is crossed by rays from Bronte, over 1700 km to the west, and Hokusai, over 2000 km to the east.

Date acquired: April 12, 2013
Image Mission Elapsed Time (MET): 8108630
Image ID: 3870271
Instrument: Narrow Angle Camera (NAC) of the Mercury Dual Imaging System (MDIS)
Center Latitude: 41.15°
Center Longitude: 289.3° E
Resolution: 22 meters/pixel
Scale: This scene is approximately 25 km (16 miles) across
Incidence Angle: 64.0°
Emission Angle: 15.0°
Phase Angle: 79.0°

Photo credit: NASA/Johns Hopkins University Applied Physics Laboratory/Carnegie Institution of Washington

Crater Cliff

The floor of the Caloris basin consists of smooth, volcanic plains -- but these plains have been modified by subsequent impacts and tectonic deformation. This crater, which is located not only on the Caloris interior plains but half-covers its neighbor, has a sharp, well-preserved rim and internal terraces. The floor of the crater is some 900 m (~0.5 mi.) below the rim, making this crater's wall quite a cliff indeed.

Date acquired: November 08, 2012
Image Mission Elapsed Time (MET): 260906527
Image ID: 1222306
Instrument: Narrow Angle Camera (NAC) of the Mercury Dual Imaging System (MDIS)
Center Latitude: 29.31°
Center Longitude: 91.0° E
Resolution: 21 meters/pixel
Scale: The field of view is ~20 km (12 mi.) across
Incidence Angle: 40.1°
Emission Angle: 8.5°
Phase Angle: 48.7°
North is to the right of this image.

Photo credit: NASA/Johns Hopkins University Applied Physics Laboratory/Carnegie Institution of Washington

Victoria Rupes

This image is a portion of the MDIS global mosaic basemap that was acquired during MESSENGER's first year in orbit. The scene, with north to the right, shows a geological feature termed Victoria Rupes -- a long cliff or scarp that formed when Mercury shrank slightly as its core cooled. Rupes on Mercury are named for ships of discovery, and Victoria Rupes is named for the Victoria that formed part of Ferdinand Magellan's fleet in his 1519-1522 effort to circumnavigate Earth.

This geologic feature is of particular interest to MESSENGER scientists because it is part of a larger, linear set of contractional structures that may correspond to what is termed a fold-and-thrust (FAT) belt on Earth. FAT belts are common terrestrial surface features, and form when the crust is shortened due to compressional tectonism. Identifying FAT belts on Mercury will help scientists understand in more detail how that planet's crust has deformed through time.

Date Created: February 10, 2012
Instrument: Wide Angle Camera (WAC) of the Mercury Dual Imaging System (MDIS)
Latitude Range: 47° N to 59° N
Longitude Range: 321° E to 331° E
Resolution: 250 meters/pixel
Scale: The crater just left of center is approximately 42 km (26 mi.) in diameter
Projection: Azimuthal equidistant

Photo credit: NASA/Johns Hopkins University Applied Physics Laboratory/Carnegie Institution of Washington

Inside Eminescu Crater

This oblique view shows a portion of the rim of the crater Eminescu. The angle of this image provides a great perspective for viewing the spectacular cliffs that formed as material slumped from the crater rim into the crater interior, as well as small ponds of impact melt perched on the rim. North is down in this image.

Date acquired: December 05, 2011
Image Mission Elapsed Time (MET): 231611014
Image ID: 1099316
Instrument: Narrow Angle Camera (NAC) of the Mercury Dual Imaging System (MDIS)
Center Latitude: 9.8°
Center Longitude: 115.5° E
Resolution: 34 meters/pixel
Scale: The scene is approximately 35 km (22 miles) from north to south.
Incidence Angle: 65.1°
Emission Angle: 60.1°
Phase Angle: 125.3°

Photo credit: NASA/Johns Hopkins University Applied Physics Laboratory/Carnegie Institution of Washington

Fram Rupes

One hundred years ago, on December 14, 1911, Norwegian explorer Roald Amundsen and his party became the first people to reach the Earth's south pole. The name of the ship that carried Amundsen to Antarctica was the Fram. The image above shows a portion of Fram Rupes on the planet Mercury, a long scarp (cliff) formed by compressive forces generated as the planet's interior cooled and contracted.

Date acquired: November 06, 2011
Image Mission Elapsed Time (MET): 229066087
Image ID: 978519
Instrument: Narrow Angle Camera (NAC) of the Mercury Dual Imaging System (MDIS)
Center Latitude: -55.5°
Center Longitude: 267.8° E
Resolution: 152 meters/pixel
Scale: The edges of the image are about 157 km long.
Incidence Angle: 67.2°
Emission Angle: 14.9°
Phase Angle: 81.2°

Photo credit: NASA/Johns Hopkins University Applied Physics Laboratory/Carnegie Institution of Washington

Long Scarp

Extending from the left edge of this image diagonally toward the lower right corner is a long scarp (cliff) face. This scarp runs through a large ancient crater in the center of the frame and was seen for the first time during MESSENGER's second Mercury flyby. Planetary geologists use the Latin term "rupes" for scarps on Mercury. Scarps such as this one have been identified all over the planet. The presence of many long and high scarps suggests a history for Mercury that is unlike that of any of the other planets in the Solar System. These giant scarps are believed to have formed when Mercury's interior cooled and the entire planet contracted slightly as a result, causing the surface rocks to fracture and some blocks of crust to thrust over others along great faults. Determining the geometry of such scarps on Mercury and information on the times that deformation occurred can thus be used to understand the thermal history of the planet. Next year, when the MESSENGER spacecraft is in orbit around Mercury, MDIS will acquire for the first time global imaging coverage of Mercury's surface with lighting conditions optimal for identifying such scarps.

Date Acquired: October 6, 2008
Instrument: Narrow Angle Camera (NAC) of the Mercury Dual Imaging System (MDIS)
Scale: The large crater crosscut by the scarp is approximately 110 kilometers (70 miles) in diameter.

Photo credit: NASA/Johns Hopkins University Applied Physics Laboratory/Carnegie Institution of Washington