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Wind, craters, and an easily eroded material have combined to produce this interesting region of features - almost looks like a scream, ala Munch!

Source: THEMIS - Mars Odyssey Mission

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Impact crater with ejecta that does not completely encircle the crater typically mean the impact occurred at an angle. The ejecta 'wings' make the crater look like a bird - or in this case perhaps an owl.

Source: THEMIS - Mars Odyssey Mission

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The ejecta around these small craters is somewhat rayed. It makes for a petal-like appearance, giving the craters the look of a bunch of daisies.

Source: THEMIS - Mars Odyssey Mission

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This VIS image shows part of the ridge located in Candor Chasma. Both wind and fluids appear to been agents of erosion in shaping the steep faces of the ridge.

Source: THEMIS - Mars Odyssey Mission

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Dark, slope steaks are common in the heavily fractured material found to the north and west of Olympus Mons.

Source: THEMIS - Mars Odyssey Mission

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Numerous small channels are found in this region of Tempe Terra.

Source: THEMIS - Mars Odyssey Mission

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When winds that have swept across the north polar ice encounter a trough in the ice the laminar flow slows at the base of the trough, producing a turbulent wind regime that is easily recognized in the clouds formed in the trough.

Source: THEMIS - Mars Odyssey Mission

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Craters with asymmetric ejecta blankets are typically formed by oblique impacts. The region of 'missing' ejecta indicates the direction of the incoming meteorite

Source: THEMIS - Mars Odyssey Mission

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Many regions in the northern plains show evidence of layered materials.

Source: THEMIS - Mars Odyssey Mission

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The many lava flows in this VIS image are part of the extensive Tharsis volcanic complex. These flows appear to originate in the region of Alba Patera and flowed downhill towards Olympus Mons.

Source: THEMIS - Mars Odyssey Mission

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This VIS image shows part of the layered deposits found in Melas Chasma.

Source: THEMIS - Mars Odyssey Mission

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This image shows some of the extensive lava flows that make up Syria Planum.

Source: THEMIS - Mars Odyssey Mission

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A small dune field covers the floor of this unnamed crater, while gullies are located on the interior of the western rim.

Source: THEMIS - Mars Odyssey Mission

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This VIS image shows lava flows and a portion of Buvinda Vallis, a channel located at the base of Hecates Tholus.

Source: THEMIS - Mars Odyssey Mission

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The eastern margin of Tempe Terra is dissected by channels of many sizes, like the one at the top of this image.

Source: THEMIS - Mars Odyssey Mission

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East of Jovis Tholus and in the midst of the Tharsis Volcanic field this dark, rayed spot is seen. Most likely this mark represents the shock wave of an incoming meteoroid that burned up before impact. The shock wave blasted the fine material away, leaving the darker basaltic surface exposed.

Source: THEMIS - Mars Odyssey Mission

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This complex surface, with intersecting linear ridges is located to the north of Nili Fossae.

Source: THEMIS - Mars Odyssey Mission

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This VIS image shows a portion of Auqakuh Vallis.

Source: THEMIS - Mars Odyssey Mission

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The top of this VIS image shows several of the many channels located on the eastern margin of Tempe Terra.

Source: THEMIS - Mars Odyssey Mission

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These dark dunes are located west of Barabashov Crater on the northern margin of Tempe Terra.

Source: THEMIS - Mars Odyssey Mission