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Canyon Junction

A false-color mosaic focuses on one junction in Noctis Labyrinthus where Mars canyons meet to form a depression 4,000 meters (13,000 feet) deep.

April 01, 2012

Credit

NASA/JPL-Caltech/University of Arizona

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Fans and ribbons of dark sand dunes creep across the floor of Bunge Crater in response to winds blowing from the direction at the top of the picture. The frame is about 14 kilometers (9 miles) wide.
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Fans and ribbons of dark sand dunes creep across the floor of Bunge Crater in response to winds blowing from the direction at the top of the picture. The frame is about 14 kilometers (9 miles) wide.
Bunge Crater Dunes
This false color image shows a region with craters of different ages located at the margin of Acidalia Planitia. This image was collected during the Northern Spring season.
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This false color image shows a region with craters of different ages located at the margin of Acidalia Planitia. This image was collected during the Northern Spring season. The THEMIS VIS camera is capable of capturing color images of the Martian surface using five different color filters. In this mode of operation, the spatial resolution and coverage of the image must be reduced to accommodate the additional data volume produced from using multiple filters. To make a color image, three of the five filter images (each in grayscale) are selected. Each is contrast enhanced and then converted to a red, green, or blue intensity image. These three images are then combined to produce a full color, single image. Because the THEMIS color filters don't span the full range of colors seen by the human eye, a color THEMIS image does not represent true color. Also, because each single-filter image is contrast enhanced before inclusion in the three-color image, the apparent color variation of the scene is exaggerated. Nevertheless, the color variation that does appear is representative of some change in color, however subtle, in the actual scene. Note that the long edges of THEMIS color images typically contain color artifacts that do not represent surface variation.
Cratered Acidalia Planitia
Marte Vallis, located in Amazonis Planitia, is broad and shallow. The streamlined islands at the top and bottom of the image illustrate this.
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Marte Vallis, located in Amazonis Planitia, is broad and shallow. The streamlined islands at the top and bottom of the image illustrate this.
Marte Vallis in Amazonis Planitia
The channels in this VIS image are part of Tyrrhena Fossae on the northern flank of Tyrrhenus Mons.
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The channels in this VIS image are part of Tyrrhena Fossae on the northern flank of Tyrrhenus Mons.
Tyrrhena Fossae
This image from NASAs Mars Odyssey shows lava flows from Alba Mons, and a tectonic graben called Cyane Fossae.
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This image from NASAs Mars Odyssey shows lava flows from Alba Mons, and a tectonic graben called Cyane Fossae.
Alba Mons
This false-color map shows the area within Gale Crater on Mars, where NASA's Curiosity rover landed on Aug. 5, 2012 PDT (Aug. 6, 2012 EDT) and the location where Curiosity collected its first drill...
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This false-color map shows the area within Gale Crater on Mars, where NASA's Curiosity rover landed on Aug. 5, 2012 PDT (Aug. 6, 2012 EDT) and the location where Curiosity collected its first drilled sample at the "John Klein" rock.
Location of John Klein Drill Site
A new map of Mars' gravity made with three NASA spacecraft is the most detailed to date, providing a revealing glimpse into the hidden interior of the Red Planet. Satellites always orbit a planet's...
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Mars Gravity Map
Mars Gravity Map
Researchers estimating the amount of carbon held in the ground at the largest known carbonate-containing deposit on Mars utilized data from three different NASA Mars orbiters.
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Researchers estimating the amount of carbon held in the ground at the largest known carbonate-containing deposit on Mars utilized data from five instruments on three different NASA Mars orbiters, including physical properties from THEMIS (left) and mineral information from CRISM (right).
Multiple Instruments Used for Mars Carbon Estimate
Researchers estimating the amount of carbon held in the ground at the largest known carbonate-containing deposit on Mars utilized data from three different NASA Mars orbiters.
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Researchers estimating the amount of carbon held in the ground at the largest known carbonate-containing deposit on Mars utilized data from five instruments on three different NASA Mars orbiters, including physical properties from THEMIS (left) and mineral information from CRISM (right).
Multiple Instruments Used for Mars Carbon Estimate
At 11:02 a.m. EDT on April 7, 2001, crowds watch a Boeing Delta II rocket lift off from Cape Canaveral Air Force Station, Florida, carrying NASA's 2001 Mars Odyssey spacecraft into space on its sev...
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At 11:02 a.m. EDT on April 7, 2001, crowds watch a Boeing Delta II rocket lift off from Cape Canaveral Air Force Station, Florida, carrying NASA's 2001 Mars Odyssey spacecraft into space on its seven-month journey to Mars.
Odyssey's Launch to Mars on April 7, 2001
This view of an area about 140 kilometers (about 90 miles) wide in the Meridiani Planum region of Mars shows the region around NASA's Mars Exploration Rover Opportunity.
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Orbital View of Opportunity's Region
Orbital View of Opportunity's Region
Sixteen seventh-graders at Evergreen Middle School in Cottonwood, Calif., found the Martian pit feature at the center of the superimposed red square in this image while participating in a program t...
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Martian Pit Feature Found by Seventh Graders
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This crater, located in Chryse Planitia, is relatively unmodified, meaning it appears very much like it did when it first formed.
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This crater, located in Chryse Planitia, is relatively unmodified, meaning it appears very much like it did when it first formed.
Lismore Crater
This graphic shows the ongoing contributions of NASA’s rovers and orbiters during a Martian dust storm that began on May 30, 2018.
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This graphic shows the ongoing contributions of NASA’s rovers and orbiters during a Martian dust storm that began on May 30, 2018.
Mars Storm Watch Observations
Large fractures have formed 'steps' in this region of Tempe Terra.
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Large fractures have formed 'steps' in this region of Tempe Terra.
Tempe Terra
This image shows two small tributaries, just east of where they join Shalbatana Vallis.
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This image shows two small tributaries, just east of where they join Shalbatana Vallis.
Shalbatana Vallis
Although this may look like a hostile alien life form, it's actually a complex line of sand dunes near the northern ice cap of Mars.
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Although this may look like a hostile alien life form, it's actually a complex line of sand dunes near the northern ice cap of Mars.
Mars Odyssey All Stars: Reptilian Dunes
Fans and ribbons of dark sand dunes creep across the floor of Bunge Crater in response to winds blowing from the direction at the top of the picture.
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Fans and ribbons of dark sand dunes creep across the floor of Bunge Crater in response to winds blowing from the direction at the top of the picture.
Mars Odyssey All Stars: Bunge Crater Dunes
This computer-generated view based on multiple orbital observations shows Mars' Gale crater as if seen from an aircraft north of the crater.
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This computer-generated view based on multiple orbital observations shows Mars' Gale crater as if seen from an aircraft north of the crater.
Oblique view of Gale Crater from the North
A vast dune field lies near the northern polar cap of Mars. Seen here in summer, the dunes have partially buried an impact crater about 1,000 meters (3,300 feet) wide.
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A vast dune field lies near the northern polar cap of Mars. Seen here in summer, the dunes have partially buried an impact crater about 1,000 meters (3,300 feet) wide.
Mars Odyssey All Stars: Dunes Engulf Crater
Olympica Fossae is a complex channel located on the volcanic plains between Alba Mons and Olympus Mons. The sinuosity of the large channel in the middle of this image from NASA's 2001 Mars Odyssey ...
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Olympica Fossae
Olympica Fossae
Stages in the seasonal disappearance of surface ice from the ground around the Phoenix Mars Lander are visible in these images taken on Feb. 8, 2010, (left) and Feb. 25, 2010, during springtime on ...
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Stages in the seasonal disappearance of surface ice from the ground around the Phoenix Mars Lander are visible in these images taken on Feb. 8, 2010, (left) and Feb. 25, 2010, during springtime on northern Mars.
Ice Around Phoenix Lander Continues to Lessen in Spring
This mosaic of day and night infrared THEMIS images shows landslides flowed over 100 kilometers (62 miles) across the floor of Melas Chasma.
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This mosaic of day and night infrared THEMIS images shows landslides flowed over 100 kilometers (62 miles) across the floor of Melas Chasma.
mosaic of day and night infrared THEMIS
At the time this video was released, the Odyssey team had successfully completed the third trajectory correction maneuver to adjust the spacecraft's flightpath toward its final aimpoint for entry i...
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Challenges of Getting to Mars: Interplanetary Cruise
Challenges of Getting to Mars: Interplanetary Cruise
The floor of this unnamed crater in Aonia Terra has been filled with multiple layers of material.
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The floor of this unnamed crater in Aonia Terra has been filled with multiple layers of material.
Layered Fill

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