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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
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
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 Sample of Pock-Marked Terrain
This difficult terrain is within a large impact crater that is side-by-side with another crater. This image is located to northwest of the Hellas impact basin in the southern latitudes of Mars.
NASA/JPL/University of Arizona (256 km above the surface, less than 5 km across.)
Source: www.uahirise.org/ESP_037516_1550
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
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)
Medusae Fossae Terrain
NASA/JPL/University of Arizona (Jun 2013, 268 km above the surface, 5 km across; www.uahirise.org/ESP_032183_1775)
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 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)
Ribbed Terrain in Deuteronilus Mensae — In addition to the ribbed terrain, there are also narrow cracks as well as upper plains material. The spots with ribbed terrain appear to be lower than the surrounding surfaces. Pictures like this may help us determine how much ice was lost from the upper plains unit in forming the ribbed terrain.
NASA/JPL/University of Arizona (304 km above the surface, less than 5 km across)
Source: www.uahirise.org/ESP_053129_2250
Apron of a Middle Fan in Ostrov Crater — These higher-standing ridges were more resistant to erosion here in Ostrov Crater, which is located in Margaritifer Terra, south of the equator. Portions of this crater look smooth in other images. (Note: the crater in this image is *not* Ostrov).
NASA/JPL/University of Arizona (258 km above the surface; scene is less than 5 km top to bottom and north is to the right.)
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
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
Charles Dickens, after his visit in 1842, wrote critically: “I am persuaded that those who designed this system... do not know what it is they are doing... I hold the slow and daily tampering with the mysteries of the brain to be immeasurably worse than any torture of the body.”
An Oblique View of Uplifted Rocks — The warm colors in this observation mark the presence of minerals altered by water.
NASA/JPL/University of Arizona (uahirise.org/ESP_021545_1660)
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
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
On the Bedrock Beauty within Verlaine Crater
NASA/JPL/University of Arizona (1 km across; www.uahirise.org/ESP_013213_1705)
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)
Aram Chaos — This is a favorite place of ours to image, located 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, less than 5 km top to bottom and north is to the right.)
Source: www.uahirise.org/ESP_016750_1830
Wide, Branching Channels – Southern spring on Mars brings sublimation of the seasonal dry ice polar cap. Gas trapped under the seasonal ice sheet carves channels on its way to escaping to the atmosphere.
NASA/JPL/University of Arizona (less than 1 km across, 250 km above the surface; www.uahirise.org/ESP_047718_0995)
Clays Exposed in a Deposit in the Electris Region: Details in clays could provide insight into how they formed.
NASA/JPL/University of Arizona (273 km above the surface)
Sediment in Jezero Crater — Beautiful lens of sediment on a meander bend.
NASA/JPL/University of Arizona (Acquired: Feb 2017, approximately 299 km above the surface. www.uahirise.org/ESP_049343_1990)
Highlands Cut by the Claritas Fossae Exhibiting Complex Mineralogy — One of the minerals here might be olivine.
NASA/JPL/University of Arizona (248 km above the suface.)
Iron and Magnesium Clays and Possible Chlorides in the Sirenum Region
NASA/JPL/University of Arizona (1 km across. uahirise.org/ESP_012865_1475)
Gully Fans on a Crater Floor
NASA/JPL/University of Arizona (Acquired: Feb 2017, approximately 258 kilometers above the surface. www.uahirise.org/ESP_049406_1555)
Exposed Bedrock Ridges in Hale Crater Ejecta — There is little to no coverage of the Hale ejecta just outside of the crater rim. This particular location has an upraised ridge which appears to be closed in by pitted material.
NASA/JPL/University of Arizona (256 km above the surface, about 5 km top to bottom and north is to the right)
Flow Margin in the Phlegra Dorsa Region
NASA/JPL/University of Arizona (Mar 2017, 291 km above the surface. Scene is less than 1 km top to bottom and north is to the right. www.uahirise.org/ESP_049722_2080)
Aging with Impacts — Counting craters to determine age estimates of planetary surfaces has been used throughout the solar system.
NASA/JPL/University of Arizona (uahirise.org/ESP_049398_2180)
Wind at Work: Wind is one of the most active forces shaping Mars' surface in today's climate.
Image: NASA/JPL/University of Arizona
A Small Channel in Lyot Crater – This channel (and others in this area) are barely visible in Context Camera images, but we can see it clearly with HiRISE resolution. What might have caused it?
NASA/JPL/University of Arizona (274 km above the surface, less than 5 km across)
Wayward in Perepelkin Crater — This crater is very old and mostly filled-in with material. It’s 112 kilometer in diameter and named after Soviet astronomer Yevgeny Perepyolkin.
NASA/JPL/University of Arizona (307 km above the surface, less than 1 km top to bottom and north is approximately to the left)
Source: www.uahirise.org/ESP_052671_2330
Each ESP controls a 5 minute slice of the clock. On boot-up, there's no connection (orange). Once connected to the WiFi network (blue), each ESP polls the currrent time with a simple HEAD Web request to google.com, then displays its part of the clock (blue or pink, minutes green). Note the "glitches" due to the independent operation of the slices (plus a programming bug in slice 0, fixed later). The red button was supposed to show a heartbeat and reset all ESPs, but there was not enough time to implement this. For this video, the clock displays seconds, instead of minutes, as does the finished version.
Source code and design files www.thingiverse.com/thing:1134525