Edited Mars Reconnaissance Orbiter image of a small mound (for unmeasured amounts of "small") mound in Chryse Planitia. Inverted grayscale variant (which makes it a lot easier to make out the details).

This VIS image shows a section of Shalbatana Vallis. Shalbatana Vallis is located in Xanthe Terra and is one of many channels that empty into Chryse Planitia.

This martian scene spans 18 x135 kilometers (11 x 84 miles). To see where on Mars this area lies, and to download high-resolution versions of the image go to themis.asu.edu/zoom-20200217a

See the Red Planet Report at redplanet.asu.edu for updates on Mars research and exploration. For more about Mars geology, check out the Mars-ePedia: marsed.asu.edu/marsepedia

For the latest THEMIS Mars images as received by mission scientists, see themis.asu.edu/livefrommars. To learn more about the THEMIS camera and its Mars images, see themis.asu.edu

This image is in the public domain and may be republished free of charge. If used, please credit it as NASA/JPL-Caltech/Arizona State University.

Winter 2014 Collection

Today's VIS image shows a section of Bahram Vallis. This channel is located in northern Lunae Planum, south of Kasei Valles. Bharam Vallis drains from the higher elevations of Lunae Planum towards the Chryse Planitia basin. This channel is over 300km long (186miles). In this image Bahram Vallis enters Waspam Crater (right side of image) and then exits the crater (top right corner).

This martian scene spans 19 x 66 kilometers (12 x 41 miles). To see where on Mars this area lies, and to download high-resolution versions of the image go to themis.asu.edu/zoom-20200622a

See the Red Planet Report at redplanet.asu.edu for updates on Mars research and exploration. For more about Mars geology, check out the Mars-ePedia: marsed.asu.edu/marsepedia

For the latest THEMIS Mars images as received by mission scientists, see themis.asu.edu/livefrommars. To learn more about the THEMIS camera and its Mars images, see themis.asu.edu

This image is in the public domain and may be republished free of charge. If used, please credit it as NASA/JPL-Caltech/Arizona State University.

"The patch of dark material toward the top of this picture (arrow) taken by the Viking 1 Lander is the debris kicked up by the impact of a protective cover ejected from the spacecraft at 1 a.m. today. The cylindrical cover, which bounced out of view of the camera, protects the scoop at the end of the soil sampler arm. (The scoop will dig into the Martian surface for the first time on July 28). Dust and debris atop the footpad remains as it was seen in the Lander's first picture taken immediately after landing two days ago. No wind modification is apparent. On the surface, a variety of block sizes, shapes and tones are seen, and some rocks are partially buried."

Also at:

photojournal.jpl.nasa.gov/catalog/PIA00384

Credit: JPL Photojournal website

The brighter region at the bottom of this VIS image is the relative highlands of Arabia Terra, while the rest of the image shows Chryse Plainitia. The boundary between the two regions is a large change in elevation as well as differences in surface texture.

The THEMIS VIS camera contains 5 filters. The data from different filters can be combined in multiple ways to create a false color image. These false color images may reveal subtle variations of the surface not easily identified in a single band image.

This martian scene spans 19 x 283 kilometers (12 x 176 miles). To see where on Mars this area lies, and to download high-resolution versions of the image, go to themis.asu.edu/zoom-20190226a

See the Red Planet Report at redplanet.asu.edu for updates on Mars research and exploration. For more about Mars geology, check out the Mars-ePedia: marsed.asu.edu/marsepedia

For the latest THEMIS Mars images as received by mission scientists, see themis.asu.edu/livefrommars. To learn more about the THEMIS camera and its Mars images, see themis.asu.edu.

This image is in the public domain and may be republished free of charge. If used, please credit it as NASA/JPL-Caltech/Arizona State University.

Winter 2014 Collection

Winter 2014 Collection

Winter 2014 Collection

Winter 2014 Collection

Winter 2014 Collection

Banh crater, within Vedra Valles, SW Chryse Planitia, Lunae Palus quadrangle. North is roughly to the top.

Winter 2014 Collection

This VIS image shows a section of Shalbatana Vallis. Located in Xanthe Terra, Shalbatana Vallis is one of many channels that empty into Chryse Planitia. Shalbatana Vallis is an outflow channel carved by massive floods from escaping groundwater whose source lies far to the south of this image. The vallis is over 1300 km long (807 miles).

This martian scene spans 18 x 66 kilometers (11 x 41 miles). To see where on Mars this area lies, and to download high-resolution versions of the image go to themis.asu.edu/zoom-201911183168a

See the Red Planet Report at redplanet.asu.edu for updates on Mars research and exploration. For more about Mars geology, check out the Mars-ePedia: marsed.asu.edu/marsepedia

For the latest THEMIS Mars images as received by mission scientists, see themis.asu.edu/livefrommars. To learn more about the THEMIS camera and its Mars images, see themis.asu.edu

This image is in the public domain and may be republished free of charge. If used, please credit it as NASA/JPL-Caltech/Arizona State University.

Today's VIS image shows a small section of Shalbatana Vallis. Located in Xanthe Terra, Shalbatana Vallis is an outflow channel carved by massive floods of escaping groundwater whose source lies far to the south of this image. This channel, and all others in this region, drain into Chryse Planitia. Shalbatana Vallis is 1029km long (639 miles).

This martian scene spans 18 x 273 kilometers (11 x 170 miles). To see where on Mars this area lies, and to download high-resolution versions of the image go to themis.asu.edu/zoom-20230704a

See the Red Planet Report at redplanet.asu.edu for updates on Mars research and exploration. For more about Mars geology, check out the Mars-ePedia: marsed.asu.edu/marsepedia

For the latest THEMIS Mars images as received by mission scientists, see themis.asu.edu/livefrommars. To learn more about the THEMIS camera and its Mars images, see themis.asu.edu

This image is in the public domain and may be republished free of charge. If used, please credit it as NASA/JPL-Caltech/Arizona State University.

Bahram Vallis crosses this VIS image. Bharam Vallis drains from the higher elevations of Lunae Planum into the Chryse Planitia basin.

At the base of several of the scalloped channel wall sections, deposits of material can be seen.

This martian scene spans 19 x 67 kilometers (12 x 42 miles). To see where on Mars this area lies, and to download high-resolution versions of the image, go to themis.asu.edu/zoom-20190724a

See the Red Planet Report at redplanet.asu.edu for updates on Mars research and exploration. For more about Mars geology, check out the Mars-ePedia: marsed.asu.edu/marsepedia

For the latest THEMIS Mars images as received by mission scientists, see themis.asu.edu/livefrommars. To learn more about the THEMIS camera and its Mars images, see themis.asu.edu.

This image is in the public domain and may be republished free of charge. If used, please credit it as NASA/JPL-Caltech/Arizona State University.

Nema crater, SW Chryse Planitia, Lunae Palus quadrangle...a little over 240 kilometers from the Viking 1 landing site. North is roughly to the upper left.

Winter 2014 Collection

FMB1190

Nombre científico: Tabebuia chrysea

Identificado por: Gentry, Alwin

País: Colombia

Departamento: La Guajira

Municipio: Maicao

NASA / JPL

NASA JPL image numbers: Viking 1-41, P-17026 (P20 Mosaic)

Image capture date: July 9, 1976

Release caption date: July 13, 1976

Viking 1 landing site.

JPL caption on the verso:

A landing site for Viking 1 has been chosen on one of the lowest regions on the surface of Mars. Center of the landing ellipse inscribed on this photomosaic of frames obtained July 9 is located at 22.4° N. Lat., 47.5° W. Long., in Chryse Planitia. It is planned to send the Viking Lander to the surface on July 20. The new location is about 740 kilometers (460 miles) northwest of the original July 4 landing site and 240 kilometers (150 miles) west of an alterate site where the spacecraft was to touch down on July 17. This area is nearly three kilometers (two miles) below Mars' mean "sea level." It is a channelled lowland northeast of the great Martian volcanoes and the Tharsis Plateau, the high altitude equatorial region. Radar scans from the Earth and pictures from the Viking Orbiter indicate it to be a reasonably safe area to attempt the landing. Viking navigation engineers predict a 99% probablility that the landing will be inside the larger ellipse--100 by 220 kilometers (62 by 137 miles). The smaller oval covers the 50% probability zone.

Vintage gelatin silver print on Kodak paper, 20.3 x 25.3, with "This Paper Manufactured By Kodak" watermarks and JPL caption affixed on the verso.

This VIS image shows a section of Shalbatana Vallis. Shalbatana Vallis is one of many channels that empty into Chryse Planitia.

This martian scene spans 19 x 66 kilometers (12 x 41 miles). To see where on Mars this area lies, and to download high-resolution versions of the image, go to themis.asu.edu/zoom-20180615a

See the Red Planet Report at redplanet.asu.edu for updates on Mars research and exploration. For more about Mars geology, check out the Mars-ePedia: marsed.asu.edu/marsepedia

For the latest THEMIS Mars images as received by mission scientists, see themis.asu.edu/livefrommars. To learn more about the THEMIS camera and its Mars images, see themis.asu.edu.

This image is in the public domain and may be republished free of charge. If used, please credit it as NASA/JPL-Caltech/Arizona State University.

Winter 2014 Collection

Mars volcanoes with Olympus Mons left of centre and clouds over Chryse and Xanthe on the right side.

Winter 2014 Collection

In planetary nomenclature, the descriptor term chaos means "distinctive area of broken terrain". The general morphology of chaos is steep-sided mesas in close proximity.

This VIS image shows a region of Chryse Chaos where the isolated mesas are beginning to be formed. The interconnected channel forms erode, and mesas are created by erosion of the bounding channels. The bottom of the image shows some of the resultant mesas.

This martian scene spans 18 x 67 kilometers (11 x 42 miles). To see where on Mars this area lies, and to download high-resolution versions of the image, go to themis.asu.edu/zoom-20180518a

See the Red Planet Report at redplanet.asu.edu for updates on Mars research and exploration. For more about Mars geology, check out the Mars-ePedia: marsed.asu.edu/marsepedia

For the latest THEMIS Mars images as received by mission scientists, see themis.asu.edu/livefrommars. To learn more about the THEMIS camera and its Mars images, see themis.asu.edu.

This image is in the public domain and may be republished free of charge, but if used it should be credited as NASA/JPL-Caltech/Arizona State University.

Viking Orbiter mosaic of western Chryse Planitia. Originally released by JPL as mosaic 211-5015.

Mars centred on Chryse and Xanthe with Sinus Sabeus creeping in lower right. Lots of faint cloud collecting with perspective effect around Tharsis Bulge and Arcadia. Mars is getting a little smaller now 3 weeks after opposition.

Winter 2014 Collection

This VIS image shows part of Hydraotes Chaos. Hydraotes Chaos measures about 300 kilometers (190 miles) wide by roughly 350 km (220 mi) north-south, and it lies in a valley leading northeast out of Ganges Chasma at the east end of Valles Marineris. Tiu Valles flows northward from Hydraotes Chaos to empty into Chryse Planitia.

This martian scene spans 18 x 66 kilometers (11 x 41 miles). To see where on Mars this area lies, and to download high-resolution versions of the image go to themis.asu.edu/zoom-20200511a

See the Red Planet Report at redplanet.asu.edu for updates on Mars research and exploration. For more about Mars geology, check out the Mars-ePedia: marsed.asu.edu/marsepedia

For the latest THEMIS Mars images as received by mission scientists, see themis.asu.edu/livefrommars. To learn more about the THEMIS camera and its Mars images, see themis.asu.edu

This image is in the public domain and may be republished free of charge. If used, please credit it as NASA/JPL-Caltech/Arizona State University.

"Courtesy NASA " processing 2di7 & titanio44

176 frame clear filter mosaic produced by Viking Orbiter 1 between July 12 and August 14, 1976. This image was produced using data from orbits 22, 44, 46, 47, 48, 50, 51 and 54.

This scene captures the large channels carved into the edge of Lunae Planum, a high plateau overlooking the Chryse Planitia lowlands. The main valley systems, from top to bottom, are Braham Vallis, Vedra Vallis, Maumee Vallis, and Maja Vallis.

Image Credit: NASA / JPL / USGS / Justin Cowart

Winter 2014 Collection

Reworked 1st Mars with surface detail, mediocre seeing, Questar 3.5, 16 mm Brandon, Sony NEX-5N eyepiece projection. 52 of 86 images 1/13 sec ASA 800 stacked and sharpened. Diameter is 13 arc seconds. The north polar ice cap is the slightly brighter spot at the bottom around 5 o’clock. The globe is centered on about 40W. The lighter area cutting from 1 to 8 o’clock is centered on Chryse, with Mare Acidalium adjoining the north ice cap, and Mare Erythraeum, the dark area in the south (11 o’clock). The large area of glare (sun on high clouds?) near 1 o’clock is to the right of the location of Valles Marineris (not resolved here - the grand canyon of Mars).

Bahram Vallis crosses this VIS image. Bharam Vallis drains from the higher elevations of Lunae Planum into the Chryse Planitia basin. Bahram Vallis is 270km (167 miles) long, with an almost uniform width along most of the channel.

This martian scene spans 19 x 67 kilometers (12 x 42 miles). To see where on Mars this area lies, and to download high-resolution versions of the image go to themis.asu.edu/zoom-20211019a

See the Red Planet Report at redplanet.asu.edu for updates on Mars research and exploration. For more about Mars geology, check out the Mars-ePedia: marsed.asu.edu/marsepedia

For the latest THEMIS Mars images as received by mission scientists, see themis.asu.edu/livefrommars. To learn more about the THEMIS camera and its Mars images, see themis.asu.edu

This image is in the public domain and may be republished free of charge. If used, please credit it as NASA/JPL-Caltech/Arizona State University.

Today's VIS image shows a portion of Shalbatana Vallis. Located in Xanthe Terra, Shalbatana Vallis is an outflow channel carved by massive floods of escaping groundwater whose source lies far to the south of this image. Shalbatana Vallis is over 1300 km long (808 miles). This channel, and all others in this region, drain into Chryse Planitia.

This martian scene spans 18 x 276 kilometers (11 x 171 miles). To see where on Mars this area lies, and to download high-resolution versions of the image go to themis.asu.edu/zoom-20210820a

See the Red Planet Report at redplanet.asu.edu for updates on Mars research and exploration. For more about Mars geology, check out the Mars-ePedia: marsed.asu.edu/marsepedia

For the latest THEMIS Mars images as received by mission scientists, see themis.asu.edu/livefrommars. To learn more about the THEMIS camera and its Mars images, see themis.asu.edu

This image is in the public domain and may be republished free of charge. If used, please credit it as NASA/JPL-Caltech/Arizona State University.

Benjamin West (1738–1820), Chryseis Returned to Her Father, 1771. Oil on canvas. New-York Historical Society, Gift of William Henry Webb, 1865.1

West took inspiration from Homer’s The Iliad to show the helmeted Odysseus returning Chryseis to her elderly father, Chryses, a priest of Apollo. The reunion takes place beneath a statue of Apollo, who had answered Chryses’ prayers for his daughter’s release from captivity at the hands of King Agamemnon. When this painting and its pendant, Aeneas and Creusa, debuted at London’s Royal Academy in 1771, these Neoclassical paintings represented the height of artistic taste

Winter 2014 Collection

Winter 2014 Collection

Winter 2014 Collection

Unterhalb des Marshochlands von Arabia Terra im Mündungsgebiet von Mawrth Vallis sind die Überreste zweier miteinander verbundener, alter Einschlagskrater von 35 Kilometer Durchmesser (im Vordergrund) bzw. 75 Kilometer Durchmesser zu erkennen. Die einst mehrere Kilometer hohen Kraterränder sind stark erodiert. Die Vertiefungen des Kraters sind fast bis zum Rand mit Ablagerungen angefüllt. In Richtung des Übergangs zum Marshochland (Bildhintergrund) sind die Kraterinnenwände mit hellen Tonmineralen bedeckt, die typisch für die Region Mawrth Vallis sind.

ESA/DLR/FU Berlin – CC BY-SA 3.0 IGO

Winter 2014 Collection

Celestron Nexstar 127 SLT

Celestron Excel 3x Barlow

Baader UV-IR Cut Filter

DMK21AU618

Captured: FireCapture - 14157 frames @ 30 fps @ f35.4

Stacking: AutoStakkert!2 - Best 70%

Wavelets: Registax 6

Postprocessing: Adobe Photoshop CS5

This VIS image shows a section of Nanedi Valles (bottom half of image). Located In Xanthe Terra, the channel system is 508 km (315 miles) long. Nanedi Valles contains two large channels that join together as the elevation drops near Chryse Planitia.

This martian scene spans 18 x 273 kilometers (11 x 170 miles). To see where on Mars this area lies, and to download high-resolution versions of the image go to themis.asu.edu/zoom-20210806a

See the Red Planet Report at redplanet.asu.edu for updates on Mars research and exploration. For more about Mars geology, check out the Mars-ePedia: marsed.asu.edu/marsepedia

For the latest THEMIS Mars images as received by mission scientists, see themis.asu.edu/livefrommars. To learn more about the THEMIS camera and its Mars images, see themis.asu.edu

This image is in the public domain and may be republished free of charge. If used, please credit it as NASA/JPL-Caltech/Arizona State University.

Winter 2014 Collection

Winter 2014 Collection

S94-43206 (8 September 1994) --- The Mars Pathfinder landing site, Ares Vallis, is in the Chryse Planitia region in the northern hemisphere of Mars. It is near the site explored by the Viking 1 Lander in 1977. The landing ellipse, 100 kilometers by 200 kilometers (60 by 120 miles) is 850 kilometers (527 miles) southeast from the Viking site. In this mosaic, made from Viking orbiter data, north is up. The mosaic shows the large outflow channels that emptied into Chryse Planitia. Ares Vallis flowed to the northwest from the southeast across the landing site. The channel formed from the release of water from the Martian subsurface and flowed across the surface creating the channels and the large islands (just to the south and northeast of the landing ellipse). The landing site itself is a very smooth depositional surface where the flood waters deposited the sediments carved from the channeling event. Landing at this location should allow the analyses of a wide variety of rock types carried by the flood.

Viking Orbiter view of fluvially modified craters near Chryse Planitia. The crater rims stand above the surrounding terrain, which created a breakwater when immense floods spilled out onto Chryse Planitia. This slowed the erosive force of water downstream, leaving terraces in the crater's wake.

Viking Orbiter 1 mosaic of the Tiu Vallis source region. Tiu Vallis, which flows over 1000 km from its source to its mouth in the plains of Chryse Planitia, appears to be related to chaotic landforms. This chaos region, similiar to those observed at the sources of other large valley networks, may have been formed by subsurface volcanic activity melting huge ice deposits.

This is a mosaic of 30 Viking Orbiter 1 images, all acquired through the spacecraft's clear filter. These images were taken during orbit 83, on September 13, 1976.

Winter 2014 Collection

ESA’s Mars Express has captured images of one of the largest outflow channel networks on the Red Planet. The Kasei Valles channel system extends around 3000 km from its source region in Echus Chasma – which lies east of the bulging volcanic region Tharsis and just north of the Valles Marineris canyon system – to its sink in the vast plains of Chryse Planitia.

A combination of volcanism, tectonics, collapse and subsidence in the Tharsis region led to several massive groundwater releases from Echus Chasma, which subsequently flooded the Kasei Valles region around 3.6–3.4 billion years ago. These ancient megafloods have left their mark on the features seen today.