Kertesz Crater Anaglyph

This is an anaglyph created from two images of the crater Kertesz. By viewing images obtained from slightly different perspectives through red-blue glasses, the brain perceives a "3-D" image. The red lens should be on the left eye. With this anaglyph, better results may be achieved by tilting the head slightly to the left. The floor of Kertesz is covered with spectacular hollows. See more images of hollows here (scroll down to "Presenter #2").

Date acquired: July 31, 2011
Image Mission Elapsed Time (MET): 220634378 and 220591163
Image ID: 575037 and 573112
Instrument: Narrow Angle Camera (NAC) of the Mercury Dual Imaging System (MDIS)
Center Latitude: 27.4°
Center Longitude: 146.1° E
Resolution: 17 meters/pixel
Scale: Kertesz crater is about 31 km (19 mi.) in diameter.
Incidence Angle: 76.4° and 75.0°
Emission Angle: 30.3° and 40.9°
Phase Angle: 106.7° and 115.9°

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

Spanish Bombs

The small crater at the left side of this image is named for Juan de Mena, a Spanish poet of the 15th century. Mena has extensive bright rays, which can be better appreciated in the global map of Mercury (right on the equator, part way in from the left). Mena formed on the rim of an existing crater, which may help to explain the asymmetric pattern of Mena's rays.

Date acquired: April 19, 2011
Image Mission Elapsed Time (MET): 211718303
Image ID: 151162
Instrument: Narrow Angle Camera (NAC) of the Mercury Dual Imaging System (MDIS)
Center Latitude: -0.24°
Center Longitude: 236.3° E
Resolution: 254 meters/pixel
Scale: The image is about 138 km (85 mi.) wide.
Incidence Angle: 65.9°
Emission Angle: 22.3°
Phase Angle: 43.6°

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

Complex Craters

While many of the most spectacular craters on Mercury are young and rayed, the vast majority are older and have been modified by both internal and external forces over time. The large 90-km crater in this image has been deformed by a lobate scarp and battered by craters up to 30 km in diameter.

Date acquired: October 27, 2011
Image Mission Elapsed Time (MET): 228200113
Image ID: 937596
Instrument: Narrow Angle Camera (NAC) of the Mercury Dual Imaging System (MDIS)
Center Latitude: 5.65°
Center Longitude: 321.9° E
Resolution: 104 meters/pixel
Scale: The large crater in this scene is approximately 90 km (56 miles) in diameter
Incidence Angle: 69.2°
Emission Angle: 66.8°
Phase Angle: 102.0°

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

Hollowed Crater

The crater at the center of this image is home to more of the "hollows" that dot Mercury's surface, which appear here as high-reflectance features near the crater's central peak and around its floor-wall boundary. This crater, which does not yet have an official name, was also seen in an early image that MESSENGER captured during the spacecraft's first imaging orbit around Mercury.

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 250-meter/pixel (820 feet/pixel) morphology base map or the 1-kilometer/pixel (0.6 miles/pixel) color base map. It is not possible to cover all of Mercury's surface at this high resolution during MESSENGER's one-year mission, but several areas of high scientific interest are generally imaged in this mode each week.

Date acquired: October 21, 2011
Image Mission Elapsed Time (MET): 227644286
Image ID: 911007
Instrument: Wide Angle Camera (WAC) of the Mercury Dual Imaging System (MDIS)
WAC filter: 7 (748 nanometers)
Center Latitude: -1.98°
Center Longitude: 354.1° E
Resolution: 337 meters/pixel
Scale: The crater at center is approximately 90 km (56 miles) across
Incidence Angle: 79.6°
Emission Angle: 56.2°
Phase Angle: 135.9°

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

Strange Hollows Discovered on Mercury

NASA's MESSENGER spacecraft has discovered strange hollows on the surface of Mercury. Images taken from orbit reveal thousands of peculiar depressions at a variety of longitudes and latitudes, ranging in size from 60 feet to over a mile across and 60 to 120 feet deep. No one knows how they got there.

"These hollows were a major surprise," says David Blewett, science team member from the Johns Hopkins University Applied Physics Laboratory. "We've been thinking of Mercury as a relic – a place that's really not changing much anymore, except by impact cratering. But the hollows appear to be younger than the craters in which they are found, and that means Mercury's surface is still evolving in a surprising way."

Mars Reconnaissance Orbiter spotted similar depressions in the carbon dioxide ice at Mars' south pole, giving that surface a "swiss cheese" appearance. But on Mercury they're found in rock and often have bright interiors and halos.

"We've never seen anything quite like this on a rocky surface."

If you could stand in one of these "sleepy" hollows on Mercury's surface, you'd find yourself, like Ichabod Crane, in a quiet, still, haunting place, with a black sky above your head.

"There's essentially no atmosphere on Mercury," explains Blewett. "And with no atmosphere, wind doesn't blow and rain doesn't fall. So the hollows weren't carved by wind or water. Other forces must be at work."

As the planet closest to the Sun, Mercury is exposed to fierce heat and extreme space weather. Blewett believes these factors play a role.

A key clue, he says, is that many of the hollows are associated with central mounds or mountains inside Mercury's impact craters. These so-called “peak rings” are thought to be made of material forced up from the depths by the impact that formed the crater. Excavated material could be unstable when it finds itself suddenly exposed at Mercury's surface.

"Certain minerals, for example those that contain sulfur and other volatiles, would be easily vaporized by the onslaught of heat, solar wind, and micrometeoroids that Mercury experiences on a daily basis," he says. "Perhaps sulfur is vaporizing, leaving just the other minerals, and therefore weakening the rock and making it spongier. Then the rock would crumble and erode more readily, forming these depressions."

MESSENGER has indeed proven Mercury unexpectedly rich in sulfur. That in itself is a surprise that's forcing scientists to rethink how Mercury was formed. The prevailing models suggest that either (1) very early in Solar System history, during the final sweep-up of the large planetesimals that formed the planets, a colossal impact tore off much of Mercury's rocky outer layering; or (2) a hot phase of the early Sun heated up the surface enough to scorch off the outer layers. In either case, the elements with a low boiling point – volatiles like sulfur and potassium – would have been driven off.

But they're still there.

"The old models just don't fit with the new data, so we'll have to look at other hypotheses."

To figure out how the planets and Solar System came to be, scientists must understand Mercury.

"It's the anchor at one end of the Solar System. Learning how Mercury formed will have major implications for the rest of the planets. And MESSENGER is showing that, up to now, we've been completely wrong about this little world in so many ways!"

What other surprises does Mercury hold? The sleepy hollows of the innermost planet may be just the beginning.

Photo credit (top):   NASA/Johns Hopkins University Applied Physics Laboratory/Carnegie Institution of Washington; (bottom):  Science/AAAS

Mapping Beethoven

At top, the white line highlights the region of Mercury's surface visible to the XRS during a solar flare on 16 June 2011. Near the center is the ~650-km-diameter Beethoven impact basin at 21° S, 236° E. This region has a higher Mg/Si ratio than the northern plains and is closer in composition to terrestrial komatiites, low-silica, high-temperature volcanic rocks that formed only very early in Earth's history.

Below, smooth plains within the same area have been mapped. In green are plains of volcanic origin. These plains display flooding and embayment relationships and color contrasts typical of volcanic plains on Mercury. Yellow denotes plains of uncertain origin. Though they may also be volcanic, they lack definitive evidence for a volcanic origin and may have formed as fluidized impact ejecta, possibly from the Beethoven impact basin, or as impact melt. In blue are plains that formed when rock was melted by impacts. Even geologically complex regions, such as the area seen here, are often dominated by volcanic deposits, and their compositions are consistent with a volcanic origin.

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

The Interior of Kuiper

The rayed crater Kuiper (11.3° S, 328.6° E), as seen by MESSENGER's wide-angle camera. The smooth regions on Kuiper's floor and to its south consist of rock that was melted by the impact that created the crater. This impact melt ponded and solidified as smooth plains. Kuiper is 62 km in diameter and is an important stratigraphic marker in Mercury's geologic history.

This image was acquired as part of MDIS's high-resolution surface morphology base map. The surface morphology base map will cover more than 90% of Mercury's surface with an average resolution of 250 meters/pixel (0.16 miles/pixel or 820 feet/pixel). Images acquired for the surface morphology base map typically have off-vertical Sun angles (i.e., high incidence angles) and visible shadows so as to reveal clearly the topographic form of geologic features.

Date acquired: May 04, 2011
Image Mission Elapsed Time (MET): 212983376
Image ID: 210557
Instrument: Wide Angle Camera (WAC) of the Mercury Dual Imaging System (MDIS)
WAC filter: 7 (748 nanometers)
Center Latitude: -12.33°
Center Longitude: 331.2° E
Resolution: 309 meters/pixel
Scale: Kuiper is 62 km (39 miles) in diameter
Incidence Angle: 78.1°
Emission Angle: 28.0°
Phase Angle: 106.1°

Photo credit:

A Northern Footprint

The X-Ray Spectrometer (XRS) on MESSENGER collects compositional information for relatively large regions on Mercury's surface, and strong signals are only received during times of high solar activity. The blue region outlined in this wide-angle camera image mosaic shows the region visible to the XRS during a solar flare on 16 April 2011. The XRS data indicates that the area is basaltic in composition, the same type of volcanic rock that comprises the lunar maria. This region is part of the vast, high-reflectance northern plains that cover approximately 6% of Mercury's surface. The 1000, 750, and 430 nm bands of the Wide Angle Camera are displayed in red, green, and blue, respectively.

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

Messenger's First Solar Day

After its first Mercury solar day (176 Earth days) in orbit, MESSENGER has nearly completed two of its main global imaging campaigns: a monochrome map at 250 m/pixel and an eight-color, 1-km/pixel color map. Apart from small gaps, which will be filled in during the next solar day, these global maps now provide uniform lighting conditions ideal for assessing the form of Mercury's surface features as well as the color and compositional variations across the planet. The orthographic views seen here, centered at 75° E longitude, are each mosaics of thousands of individual images. At right, images taken through the wide-angle camera filters at 1000, 750, and 430 nm wavelength are displayed in red, green, and blue, respectively.

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

A View Towards the Plains

This view was captured as MDIS pointed to the east, which is oriented as the top of this image. Smooth plains extend into the distance, while the closer ground near the bottom of the image is more heavily cratered and hence rougher in texture. This location is on the edge of volcanic smooth plains that covers a great extent of Mercury's northern region.

Date acquired: August 12, 2011
Image Mission Elapsed Time (MET): 221626724
Image ID: 622112
Instrument: Wide Angle Camera (WAC) of the Mercury Dual Imaging System (MDIS)
WAC filter: 7 (748 nanometers)
Center Latitude: 62.40°
Center Longitude: 321.6° E
Resolution: 242 meters/pixel
Scale: The bottom of this image is 220 kilometers (140 miles) across
Incidence Angle: 82.5°
Emission Angle: 59.4°
Phase Angle: 142.0°

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

Double Ring Impact Basin

This image shows a double ring impact basin with a smaller, younger crater superimposed on its rim. Larger impacts, such as the one that created this basin, form ring structures instead of central peaks.

Date acquired: June 02, 2011
Image Mission Elapsed Time (MET): 215511113
Image ID: 329264
Instrument: Narrow Angle Camera (NAC) of the Mercury Dual Imaging System (MDIS)
Center Latitude: -80.35°
Center Longitude: 212.0° E
Resolution: 255 meters/pixel
Scale: The large impact crater is ~165 km (102 mi) in diameter.
Incidence Angle: 81.6°
Emission Angle: 0.9°
Phase Angle: 82.2°

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

Debussy Crater Rays and a Cosmic Ray

The rays apparent in this spectacular limb image of Mercury come from Debussy, the sharp crater near the terminator. This dominant crater on Mercury was also a part of MESSENGER's historic image of Mercury - the first image ever to be taken from a spacecraft in orbit about this planet. Readers may also notice a streak in the blackness of space in the top right corner of the image. This artifact was produced by a cosmic ray hitting the camera's CCD detector while the image was being collected.

Date acquired: July 26, 2011
Image Mission Elapsed Time (MET): 220137668
Image ID: 550504
Instrument: Wide Angle Camera (WAC) of the Mercury Dual Imaging System (MDIS)
WAC filter: 7 (748 nanometers)
Center Latitude: -27.90°
Center Longitude: 29.17° E
Resolution: 2783 meters/pixel
Scale: Mercury's radius is approximately 2440 km (1516 miles)
Incidence Angle: 65.1°
Emission Angle: 48.2°
Phase Angle: 95.3°

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

Ts'ai Wen-Chi Crater and the Long Scarp

A long scarp runs vertically through the center of this image, deforming pre-existing craters along its length. At the bottom of this image, the scarp cuts through the wall and floor of the crater Ts'ai Wen-Chi (124 km diameter), named for the Han Dynasty poet and composer.

Date acquired: August 04, 2011
Image Mission Elapsed Time (MET): 220977824
Image ID: 591397
Instrument: Wide Angle Camera (WAC) of the Mercury Dual Imaging System (MDIS)
WAC filter: 7 (748 nanometers)
Center Latitude: 27.73°
Center Longitude: 337.4° E
Resolution: 432 meters/pixel
Scale: This image is approximately 600 km (370 miles) across
Incidence Angle: 81.9°
Emission Angle: 38.2°
Phase Angle: 120.2°

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

Uncharted Territory

This image, captured by the Narrow Angle Camera (NAC), shows a crater in a region of Mercury not seen by Mariner 10. This crater was first imaged during MESSENGER's Mercury flybys, but this is the first image to reveal its detailed morphology. The crater's name will be chosen in accordance with a set of rules established by the International Astronomical Union (available here). Craters on Mercury are named after deceased artists, musicians, painters or authors who have made outstanding contributions to their fields and who have been considered a historically significant figure for at least 50 years.

Date acquired: July 20, 2011
Image Mission Elapsed Time (MET): 219646866
Image ID: 527953
Instrument: Narrow Angle Camera (NAC) of the Mercury Dual Imaging System (MDIS)
Center Latitude: 6.70°
Center Longitude: 38.52° E
Resolution: 193 meters/pixel
Scale: This crater is about 113 km (70 miles) in diameter
Incidence Angle: 71.4°
Emission Angle: 15.1°
Phase Angle: 56.2°

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

Double Trouble

This image, taken by the Narrow Angle Camera (NAC), shows the double rings of an unnamed peak-ring basin. Concentric ring structures like these form during the impact that creates a basin; the number and characteristics of the rings depend on the size of the impact structure and the gravity of the planet.

Date acquired: July 20, 2011
Image Mission Elapsed Time (MET): 219644470
Image ID: 527930
Instrument: Narrow Angle Camera (NAC) of the Mercury Dual Imaging System (MDIS)
Center Latitude: -17.66°
Center Longitude: 45.56° E
Resolution: 175 meters/pixel
Scale: The large double ring basin is about 172 km (107 miles) in diameter.
Incidence Angle: 65.6°
Emission Angle: 0.7°
Phase Angle: 66.1°

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

Happy Trails

This view, captured by the Wide Angle Camera (WAC), shows a trail of small craters. Such secondary crater chains are formed when the ejecta from a primary impact fall in the surrounding area, forming their own often overlapping small craters. Also visible in this image are smooth plains, formed by volcanism that has filled in a large impact crater.

Date acquired: July 15, 2011
Image Mission Elapsed Time (MET): 219181924
Image ID: 505807
Instrument: Wide Angle Camera (WAC) of the Mercury Dual Imaging System (MDIS)
WAC filter: 7 (748 nanometers)
Center Latitude: 83.21°
Center Longitude: 173.6° E
Resolution: 155 meters/pixel
Scale: The small crater at the bottom of the image has a diameter of 24 km (15 miles).
Incidence Angle: 85.3°
Emission Angle: 0.2°
Phase Angle: 85.3°

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

Crater Captivation

This image, captured by the Narrow Angle Camera (NAC), shows an unnamed complex crater in Mercury's southern hemisphere. The smooth crater floor is likely due to impact melt that formed during the collision that produced the crater. Also visible are the peak ring and terraced walls, as well as the ejecta blanket and a large field of secondary craters and crater chains.

Date acquired: July 25, 2011
Image Mission Elapsed Time (MET): 220043917
Image ID: 546489
Instrument: Narrow Angle Camera (NAC) of the Mercury Dual Imaging System (MDIS)
Center Latitude: -66.40°
Center Longitude: 81.43° E
Resolution: 326 meters/pixel
Scale: The large crater has a diameter of about 155 km (96 miles)
Incidence Angle: 67.0°
Emission Angle: 33.5°
Phase Angle: 100.5°

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

Rembrandt Revisited

This limb image shows Rembrandt, the second largest impact basin on Mercury after Caloris. Discovered during the second MESSENGER flyby, Rembrandt is one of the youngest impact basins on Mercury, as indicated by the relatively low density of impact craters on its rim. A large lobate scarp trending from the southwest to the north crosscuts Rembrandt and several of the smaller craters that have impacted the smooth interior plains.

Date acquired: August 07, 2011
Image Mission Elapsed Time (MET): 221198580
Image ID: 601688
Instrument: Wide Angle Camera (WAC) of the Mercury Dual Imaging System (MDIS)
WAC filter: 7 (748 nanometers)
Center Latitude: -32.95°
Center Longitude: 84.90° E
Resolution: 1756 meters/pixel
Scale: The large impact basin is ~715 km (444 mi) in diameter.
Incidence Angle: 46.3°
Emission Angle: 48.7°
Phase Angle: 95.0°

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

Impact Crater on the Edge of Oskison Crater

This image features a crater situated at the edge of the larger Oskison crater located in the plains north of Caloris basin. Due to MESSENGER's highly elliptical orbit, MDIS's Wide Angle Camera is capable of capturing higher resolution images in Mercury's northern hemisphere, such as this 58 meters per pixel view. A detailed look at the crater reveals its terraced walls, smooth floor, and its superposition on Oskison's shadowed rim.

Date acquired: August 01, 2011
Image Mission Elapsed Time (MET): 220677117
Image ID: 577219
Instrument: Wide Angle Camera (WAC) of the Mercury Dual Imaging System (MDIS)
WAC filter: 7 (748 nanometers)
Center Latitude: 60.18°
Center Longitude: 141.9° E
Resolution: 58 meters/pixel
Scale: This crater is approximately 39 km (24 mi) in diameter.
Incidence Angle: 81.2°
Emission Angle: 0.8°
Phase Angle: 80.5°

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

Firdousi Crater and Region

This image shows a portion of Mercury's surface mainly consisting of smooth plains material. This lighter, smoother area of plains is younger than the darker, rougher surrounding terrain near the edges of this image. Firdousi crater and its halo of small secondary craters is also apparent in this image, in the lower left quadrant.

Date acquired: July 17, 2011
Image Mission Elapsed Time (MET): 219349510, 219349512, 219349518
Image ID: 513659, 513658, 513662
Instrument: Wide Angle Camera (WAC) of the Mercury Dual Imaging System (MDIS)
WAC filter: 9 (1000 nanometers), 7 (750 nanometers), 6 (433 nanometers) as red-green-blue
Center Latitude: 6.77°
Center Longitude: 69.01° E
Resolution: 1330 meters/pixel
Scale: The large crater in the lower left quadrant of this image is about 134 kilometers (80 miles) in diameter
Incidence Angle: 52.4°
Emission Angle: 0.3°
Phase Angle: 52.4°

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