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Valleys and Layering along Melas Chasma
NASA/JPL/University of Arizona (less than 1 km across; www.uahirise.org/ESP_013983_1705)
Possible Hydrated Minerals between Scylla Scopulus and Charybdis Scopulus — Scylla Scopulus is an escarpment that is located opposite to Charybdis Scopulus and runs opposite to each other.
NASA/JPL/University of Arizona (255 km above the surface. Black and white is less than 5 km across).
www.uahirise.org/ESP_013940_1520
Slopes of Layered Deposits – This is one of our favorite areas to image, as the rocky outcrops almost look like islands in a dune sea. The area is directly north of the Valles Marineris canyon system.
NASA/JPL/University of Arizona (Acquired: November 2016, approximately 276 kilometers above the surface. Scene is 5 km across. www.uahirise.org/ESP_048372_1715)
Layering in Walls in a Depression in Nereidum Montes – This depression lies within a large (over 5 km wide) impact crater.
NASA/JPL/University of Arizona (257 km above the surface, 5 km across)
Possible Clays on the Plains near Margaritifer Chaos
NASA/JPL/University of Arizona (265 km above the surface, less than 5 km across)
Source: www.uahirise.org/ESP_018794_1695
A Possible Alluvial Fan: Fan-shaped lobes likes these are also in the desert southwest of the United States, and are called "alluvial fans."
Image: NASA/JPL/University of Arizona
A Fluvial Feature to the North of Hellas Planitia — The high-standing ridges suggest that their material is more resistant to the surrounding terrain.
NASA/JPL/University of Arizona (262 km above the surface and the scene is 5 km across).
Dark Material in a Crater in the Arabia Region
NASA/JPL/University of Arizona (Mar 2013, 285 km above the surface; less than 1 km top to bottom, and North is to the right; www.uahirise.org/ESP_031254_1965)
At the Peak of Baldet Crater in the Nili Fossae Region
NASA/JPL/University of Arizona (1 km across; www.uahirise.org/ESP_016127_2030)
Chaos Terrain
NASA/JPL/University of Arizona (273 km above the surface, less than 5 km across)
Source: www.uahirise.org/ESP_053145_1800
No Rain Falls on This Plain
This image is in Noachis Terra, an extensive southern landmass to the west of the Hellas impact basin.
NASA/JPL/University of Arizona (258 km above the surface, less than 5 km across.)
Source: www.uahirise.org/ESP_020242_1620
The Pits of Elysium Mons
The chain of pits likely formed by volcanic processes, such as the collapse of a lava tube after it drained.
Read the full caption: uahirise.org/ESP_056026_2050
NASA/JPL/University of Arizona
Slope Monitoring in Hale Crater's Central Peaks
NASA/JPL/University of Arizona
(Acquired: December 2016, approximately 252 kilometers above the surface. Enhanced color scene is less than 1 km across; www.uahirise.org/ESP_048530_1440)
Light-Toned Material in Aram Chaos – Aram Chaos mainly comprises a heavily eroded impact crater on Mars. It lies at the eastern end of the large canyon Valles Marineris and close to Ares Vallis. Various geological processes have reduced it to a circular area of chaotic terrain.
NASA/JPL/University of Arizona (274 km above the surface. Black and white is less than 5 km across and north is to the right)
Source: www.uahirise.org/ESP_016539_1830
Medusae Fossae Terrain
NASA/JPL/University of Arizona (Jun 2013, 268 km above the surface, 5 km across; www.uahirise.org/ESP_032183_1775)
Standing above It All — This is within Mclaughlin Crater, where possible delta deposits are located. If accurate, the delta would have been created hundreds of millions of years ago.
NASA/JPL/University of Arizona (Acquired: November 2016, approximately 288 kilometers above the surface. Scene is less than 1 km across. www.uahirise.org/ESP_048371_2025)
Possible Carbonate-Rich Terrain in the Northeast Syrtis Region Basin
NASA/JPL/University of Arizona (279 km above the surface, less than 5 km across.)
Source: www.uahirise.org/ESP_023735_1980
Rising Above It in Amazonis Planitia
How did this feature get here if it looks so different than its surroundings?
Read the full caption: uahirise.org/ESP_055022_2035
NASA/JPL/University of Arizona
Outcrops in Mawrth Vallis
One of the oldest valleys on Mars, Mawrth Vallis holds special interest because of the presence of clay minerals which form only in the presence of water.
NASA/JPL/University of Arizona (284 km above the surface, less than 5 km across)
Source: www.uahirise.org/ESP_016486_2000
Gullies in a Crater along a Trough Near Mariner Crater
The objective of this observation is to examine gullies in a crater that sits on the edge of a trough. Gullies are found at other places along this trough system, so by imaging these craters we can determine the the nature of the layer that is producing the gullies.
NASA/JPL/University of Arizona (254 km above the surface. Scene is 5 km across. www.uahirise.org/ESP_050038_1435)
Rocky Bedrock Southwest of Ganges Chasma
NASA/JPL/University of Arizona (Less than 1 km across, www.uahirise.org/ESP_014259_1680)
A Young, Fresh Crater in Hellespontus: At 1.3 kilometers in diameter, this unnamed crater is only slightly larger than Arizona's Meteor Crater. (NASA/JPL/University of Arizona)
An ExoMars Landing Site
HiRISE plays an important role in finding suitable landing sites for future rover missions. Scientists have narrowed down the candidate landing sites for the upcoming European ExoMars rover mission to two regions: the plains of Oxia and Mawrth Vallis.
HiRISE pictures help to assess the risk for each particular location so that a final landing site can be selected.
NASA/JPL/University of Arizona
Source: www.uahirise.org/ESP_056916_1990
The Eastern Rim of a Crater in Tyrrhena Terra with a Possible Olivine Signature
NASA/JPL/University of Arizona (Acquired: Feb 2017, approximately 259 kilometers above the surface. Less than 1 km from top to bottom and North is to the right. uahirise.org/ESP_049462_1625)
Frederick Festival of the Arts - For videos see: www.frederick.com/frederick-festival-of-the-arts
photos by Frederick.com
Layered Bedrock in the Meridiani Region (Mars)
Prior to acquiring this observation of the Meridiani region in 2010, we didn’t have any images of this particular area. It was also selected as good place for a nadir observation, which is when the camera is pointing straight down.
NASA/JPL/University of Arizona (270 km above the surface, less than 1 km top to bottom and north is to the right.)
Source: www.uahirise.org/ESP_016248_1820
To Catalog the Dunes – Believe it or not, the United States Geological Survey does enter these dunes into a global dune database. The reason? “ Dunes are particularly suited to comprehensive planetary studies because they are abundant over a wide range of elevations and terrain types. Thus a global scale study of Martian dunes serves a dual purpose in furthering understanding of both climatic and sedimentary processes.”
Sounds good to us!
NASA/JPL/University of Arizona (251 km above the surface, less than 5 km top to bottom and north is to the right)
Source: www.uahirise.org/ESP_019287_1180
Tell-Tale Bedrock in Tyrrhena Terra — Geologists study the central peaks of craters because the uplifted bedrock was once deep within the Martian crust.
Read the caption here: uahirise.org/ESP_055238_1615
NASA/JPL/University of Arizona
Possible Well-Exposed Ejecta of a Crater in Noachis Terra — The exposure of the ejecta as well as possible breccia (large, jumbled rocks) are at a fine scale in this image.
NASA/JPL/University of Arizona (256 km above the surface. Enhanced color is less than 1 km top to bottom and north is to the right.)
Twin Craters in Meridiani Planum — This image is an example of the principle of superposition: figuring out what happened first by looking at how features interact with each other.
NASA/JPL/University of Arizona (273 km above the surface, less than 5 km across)
Barchan Dunes in Dulovo Crater
NASA/JPL/University of Arizona (274 km above the surface. Black and white is less than 5 km top to bottom and north is to the right.)
Source: www.uahirise.org/ESP_019357_1835
A Pit in a Mid-Latitude Crater Wall
NASA/JPL/University of Arizona (Apr 2011, 250 km above the surface, less than 5 km across; www.uahirise.org/ESP_022310_1285)