Radar Bright Deposits in Mercury's Polar Craters
A radar image of Mercury's north polar region is shown superposed on a mosaic of MESSENGER images of the same area. All of the larger polar deposits are located on the floors or walls of impact craters. Deposits farther from the pole are seen to be concentrated on the north-facing sides of craters. These polar deposits have been hypothesized to consist of water ice.
NASA/Johns Hopkins University Applied Physics Laboratory/Carnegie Institution of Washington
Solar Storm Affects Mercury Imagery
In March 2012, a powerful solar storm affected MESSENGER's imagery. In this picture of Mercury's surface, the bright streaks and speckles result from energetic particles from the Sun hitting the charged-couple device (CCD) on the spacecraft's camera. Images acquired during the storm will have to be taken again later in the mission.
NASA/Johns Hopkins University Applied Physics Laboratory/Carnegie Institution of Washington
Landslides on Mercury
This impact crater, approximately 25 km (16 miles) in diameter, has been heavily modified by landslides. Portions of the crater's walls detached and slumped towards the floor, producing terraces along the wall, landslide deposits on the crater floor, and modifying the crater's outline from circular to irregular. The small bright spots on the landslide deposits (near the top of the image) may be hollows, similar to those seen in other impact craters on Mercury.
NASA/Johns Hopkins University Applied Physics Laboratory/Carnegie Institution of Washington
Mercury’s Peak-Ring Basins
Two prominent basins, Chekhov at the upper left and Schubert at lower right, are both just under 200 km in diameter but have very different appearances. Chekhov has a prominent peak ring and its older age is reflected in the numerous craters that have battered its rim and floor. Schubert's floor is smooth with only a hint of its peak ring peeking through.
NASA/Johns Hopkins University Applied Physics Laboratory/Carnegie Institution of Washington
Mercury's Scarps
A common tectonic feature found on Mercury is a scarp, or steep cliff, such as the one extending across the length of this image. Though common on Mercury, long, globally distributed scarps like this are not common on the other planets in the solar system. It is believed that the scarps formed due to Mercury's thermal history. This image was acquired by the MESSENGER spacecraft as a high-resolution targeted observation on December 31, 2011.
NASA/Johns Hopkins University Applied Physics Laboratory/Carnegie Institution of Washington
MESSENGER Explores Mercury - In Color
During MESSENGER's second flyby of Mercury, the Mercury Dual Imaging System (MDIS) acquired a strip of high-resolution images obtained with each of the Wide Angle Camera's (WAC) 11 different color filters. The graphic shown here displays the resulting enhanced-color mosaic.
NASA/Johns Hopkins University Applied Physics Laboratory/Carnegie Institution of Washington
Mercury - Spectacular Color
This spectacular color mosaic shows the eastern limb of Mercury as seen by MESSENGER as the spacecraft departed the planet following the mission's first Mercury flyby in January 2008. The colors of this image are not those that would be seen by the human eye but instead convey information about the distribution of different rock types on Mercury's surface. The Caloris basin, visible as a large bright yellow circular area in this image due to its infill of volcanic plains, dominates the northern region.
NASA/Johns Hopkins University Applied Physics Laboratory/Carnegie Institution of Washington
Mercury - Crater Ejecta and Chains of Secondary Impacts
This newly observed flat-floored crater was viewed at an oblique angle as the MESSENGER spacecraft approached Mercury for its third flyby, about two hours from closest approach. This crater is younger than nearby craters of similar size, indicated by the distinctive halo of small secondary craters that radiate outward from the central structure. Many of these secondaries are aligned in chain-like formations. Crater chains are just one of many ejecta types observed on Mercury.
NASA/Johns Hopkins University Applied Physics Laboratory/Carnegie Institution of Washington
Volcanism on Mercury
The mosaic, which shows the western limb of the planet with north to the right, was assembled from individual NAC images acquired as the MESSENGER spacecraft approached the planet during the second Mercury flyby. Visible in the mosaic are many lava-flooded craters and large expanses of smooth volcanic plains, which appear similar in texture to volcanically emplaced mare deposits on the Moon.
NASA/Johns Hopkins University Applied Physics Laboratory/Carnegie Institution of Washington
A Color View of the Solar System's Innermost Planet - Mercury
As MESSENGER approached Mercury for the mission's third and final flyby of the solar system's innermost planet, the WAC acquired images through all 11 of its narrow-band color filters. The 1,000, 700, and 430 nanometer filters were combined in red, green, and blue to create this color image, the last close-up color view that was acquired before MESSENGER went into orbit around Mercury in March of 2011. Only 6 percent of Mercury's surface in this image had not been viewed previously by spacecraft, and most of the measurements made by MESSENGER's other instruments during this flyby were made prior to closest approach. The observations from MESSENGER's third flyby of Mercury nonetheless revealed fresh surprises.
NASA/JPL
This mosaic shows the planet Mercury as seen by Mariner 10 as it sped away from the planet on March 29, 1974. The mosaic was made from over 140 individual TV frames taken about two hours after encounter, at a range of 37,300 miles (60,000 kilometers). North is at top. The limb is at right, as is the illuminating sunlight. The equator crosses the planet about two-thirds of the way from the top of the disc. The terminator, line-separating day from night, is about 190 degrees west longitude. The planet shows a gibbous disc-more than half-illuminated. This hemisphere is dominated by smooth plains, rather than heavily cratered terrain, and resembles portions of the Moon's maria in general shape. Half of a very large, multi-ringed basin named Caloris Basin appears near the center of the disc near the terminator. Its surrounding mountain ring is 800 miles (1,300 kilometers) in diameter.
Mariner 10
MESSENGER
Shaded Relief Maps
Geologic Maps
Shaded Relief & Surface Markings
Reference Mosaic
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About Mercury
Spacecraft/Missions
Online Imagery
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