Determining when the light-toned layered deposits formed is important for understanding the geologic history of Valles Marineris, especially because these deposits are hydrated and most likely formed in the presence of liquid water.

Narration: Tre Gibbs
https://uahirise.org/ESP_070107_1750

When Did the Light-Toned Layers Form?

Based on their shapes and examples of fractured crests in some areas, mega-ripples are thought to be largely inactive relics of past climates.

Narration: Tre Gibbs

https://uahirise.org/ESP_053345_2640
NASA/JPL-Caltech/UArizona

Marvelous Martian Mega-Ripples

This image shows a variety of wind-related features near the center of Gamboa Crater. Larger sand dunes form sinuous crests and individual domes.

Narration: Tre Gibbs

https://uahirise.org/ESP_073613_2210
NASA/JPL-Caltech/UArizona

Piles of Sand with Different Sizes and Colors

This feature looks a bit like a bear’s face. What is it really?

Narrated by Tre Gibbs.

https://uahirise.org/ESP_076769_1380
NASA/JPL-Caltech/UArizona
#Mars #science #NASA

A Bear on Mars?

Gullies lying on the northeast slopes of Triolet Crater (about 11.6 km in diameter ), are located in the Southern Highlands just east of Gorgonum Chaos. Some gullies have eroded through resistant layers up to the crater rim.

Narration: Tre Gibbs

https://uahirise.org/ESP_075886_1425
NASA/JPL-Caltech/UArizona
#Mars #science #NASA

Multiple Episodes of Gully Activity in Triolet Crater

Harmakhis Vallis is an approximately 800-kilometer long outflow channel located in eastern Hellas. The valley probably formed by a combination of surface collapse and flowing water.

Narration: Tre Gibbs

https://uahirise.org/hipod/ESP_075639_1420
NASA/JPL-Caltech/UArizona

Going with the Flow

This impact disturbed dust over an area more than two kilometers wide, large enough to be visible in MARCI daily global images. The largest new crater is about 35 meters in diameter, making it the about the 16th largest new crater found on Mars.

Narration: Tre Gibbs

https://uahirise.org/ESP_076590_2180
NASA/JPL-Caltech/UArizona

A New Impact Event

The surface of Mars is littered with examples of glacier-like landforms. While surface ice deposits are mostly limited to the polar caps, patterns of slow, viscous flow abound in many non-polar regions of Mars.

Narration: Tre Gibbs

https://uahirise.org/ESP_078292_2175
NASA/JPL-Caltech/UArizona
#Mars #science #NASA

Icy Flows

This image shows the transition from a regular channel to an inverted channel in Arabia Terra. The channel was once flowing with water that carved down into the bedrock to produce a depression.

Narration: Tre Gibbs

https://uahirise.org/ESP_078858_2120
NASA/JPL-Caltech/UArizona
#Mars #science #NASA

From Low to High Channels

Many of the Valles Marineris canyons, called chasmata, have kilometer-high, light-toned layered mounds made up of sulfate materials. Ius Chasma, near the western end of Valles Marineris, is an exception.

Narration: Tre Gibbs

https://uahirise.org/ESP_078863_1710
NASA/JPL-Caltech/UArizona
#Mars #science #NASA

Light-Toned Materials along the Floor and Walls of Ius Chasma

This image shows the southern wall of Coprates Chasma, in the equatorial canyon system of Valles Marineris. While much of the lower slopes are covered by sand, exposed bedrock is clearly visible in the upper canyon walls.

Narration: Tre Gibbs

https://uahirise.org/ESP_079482_1650
NASA/JPL-Caltech/UArizona
#Mars #science #NASA

Diverse Minerals in Coprates Chasma

HiRISE (High Resolution Imaging Science Experiment) is the most powerful camera ever sent to another planet: Mars! We're one of six instruments onboard the MRO spacecraft, offering up audio of our captioned images release.

When Did the Light-Toned Layers Form?

BeautifulMars (HiRISE/NASA)

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