Images of and on the planet Mars.
Lunar and Planetary Institute
Different Types of Gullies
The powerful Mars Reconnaissance Orbiter HiRISE camera reveals many details of gullies that have never been seen before. Some hypotheses about the formation of gullies involve the flow of some amount of liquid (water, brine, or some other substance), and others postulate that gullies could be formed by the downhill movement of dry material such as dust or sand. To further complicate things, different gullies could have formed by different methods.
Rifts on Venus, Earth, and Mars
This is a comparison of rift zones on the three largest terrestrial planets. The Venus radar image is of Devana Chasma. On Earth, digital topography and bathymetry display a shaded relief portrayal of the East African rift system as it intersects at the Afar Triangle. The Mars image is of the Valles Marineris system. Prepared by Robert Herrick.
Jezero Crater’s Ancient Lakeshore and Minerals
In the image at left, the lighter colors represent higher elevation in this image of Jezero Crater on Mars, the landing site for NASA’s Mars 2020 mission, which is targeting a probable delta and lake shoreline. At right, color has been added to highlight minerals in this image of Jezero Crater on Mars. The green color represents minerals called carbonates, which are especially good at preserving fossilized life on Earth. Red represents olivine sand eroding out of carbonate-containing rocks.
Olympus Mons, Mars-Hawaii Comparison
The martian volcano Olympus Mons is one of the largest volcanos in the solar system, measuring over 600 km across & rising more than 27 km above the surrounding plain. In this view, Olympus Mons is compared to the Hawaiian Islands, & demonstrates the value of comparative planetary volcanology. Notice that the Island of Oahu would easily fit inside the summit caldera of the martian volcano.
A Martian Meteorite
This meteorite, EETA 79001, found on the ice in Antarctica, & is almost certainly from Mars. The cube at the lower right is 1 cm on a side. The meteorite is partly covered by a black glassy layer, the fusion crust. Inside, the meteorite is gray. It is a basalt, very similar to basalts found on Earth. It formed in a volcanic eruption about 180 million years ago. This meteorite contains a small amount of gas that is chemically identical to the martian atmosphere.
Planetary Petrology. Panel 4. Water on Mars.
Liquid water is required for life as we currently know it, therefore finding evidence for water has been a high priority for martian exploration. My book focuses on evidence for water and other volatile elements in the martian crust and what that means for the potential habitability of Mars.
Planetary Petrology. Panel 2. Mars on Earth
Examining features on Earth similar to those on Mars can provide insights as to how those features formed. The Colorado Plateau in Utah has similar features to Gusev Crater & Jezero Crater. At our field site, lava (dark gray in the picture) intruded sulfur-rich sediments. The lava provided heat to the area around it, causing groundwater to heat up and form a hydrothermal system. The hydrothermal system could have been a habitable environment on Earth & by extension on Mars.
Comparison of Volcanos on Venus and Mars
The image on the left is a Magellan radar image of Sapas Mons, one of the larger venusian volcanos, shown at the same scale as a Viking image mosaic of Olympus Mons, the largest volcano on Mars. The two volcanos are comparable in diameter, but Sapas Mons rises only 4 km above the surrounding plains while Olympus Mons is more than 20 km high. Prepared by Robert Herrick.
Panorama of Curiosity's Belly Check
This view of the lower front & underbelly areas of NASA's Mars rover Curiosity combines 9 images taken by the rover's Mars Hand Lens Imager during the 34th Martian day, or sol, of Curiosity's work (Sept. 9, 2012). Curiosity's front Hazard-Avoidance cameras appear as a set of 4 blue eyes at the top center. Fine-grain Martian dust can be seen adhering to the wheels, which are about 16 inches wide & 20 inches in diameter. The bottom of the rover is about 26 inches above the ground.
Mars Rocks Continue to Fascinate
This microscopic image of a drill hole cut into a martian rock nicknamed "Ice Cream" by the rover's rock abrasion tool shows cross sections of round concretions 0.04 to 0.08 inches wide. Science team members are debating whether the grayish-looking smudges that are not as round are concretions or some other feature. Opportunity took this mosaic of images with its microscopic imager on Aug. 6, 2005. The area shown is approximately 2.4 inches wide.
Looking Back at ‘Purgatory Dune’
The wheels of NASA's Mars Exploration Rover Opportunity dug more than 4 inches deep into the soft, sandy material of a wind-shaped ripple in Mars' Meridiani Planum region during the rover's 446th martian day, or sol (April 26, 2005). Opportunity used its navigation camera to capture this look back at the ripple during sol 491 (June 11, 2005), a week after the rover drove safely onto firmer ground. The ripple that became a sand trap is about one foot tall and 8 feet wide.
Size Comparison, Mars Science Laboratory and Mars Exploration Rover
An artist's concept of NASA's Mars Science Laboratory (left) serves to compare it with Spirit, one of NASA's twin Mars Exploration Rovers. The images of Spirit and the more advanced rover are both superimposed by special effects on a scene from Mars' "Columbia Hills," photographed by Spirit's panoramic camera on April 13, 2005, and presented here in false color
Have a Happy Mars
The Mars Reconnaissance Orbiter Context Camera has been acquiring 6 meters (19.7 feet) per pixel images of Mars since Oct. 2006. To date, more than 20% of Mars has been covered at this scale, and at least 1% more is added each month. This picture of a crater resembling a “happy face” was acquired on 28 January 2008. The unnamed crater is about 1.9 miles across. It is located among the Nereidum Montes, north of the Argyre basin, near 45.1°S, 55.0°W. North is toward toward the right.
Viking 1 Landing Site - Corrected, Mars
Viking 1 landed near two outflow channels that emptied into Chryse Planitia. Floodwaters from these channels probably flowed over this site. Later the martian winds formed dunes in the area. This corrected version of the scene allows the viewer to scan most of the scene in front of the lander. Several small ridges now stand out sharply in the middle foreground. This view exaggerates the relief. In some areas, the horizon may actually appear nearer than the foreground objects.
Sand-laden jets shoot into the polar sky in this view by noted space artist Ron Miller. It shows the Martian south polar ice cap as southern spring begins. The explosive model depicted in this artwork is a possible explanation for the seasonal, dark spider-like deposits observed at the Martian south pole.