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Mars Reconnaissance Orbiter : HiRISE Instrument captured this fantastic, Abstract Artwork created by dust devils on Mars in the Dune Fields of Hellas Planitia back in 2010.
Source Data :
hirise.lpl.arizona.edu/ESP_016483_1360
Original Image Credit: NASA / JPL / University of Arizona
Adjusted / Processed image credit: Neal Spence
Aonia Terra Dune Field
NASA/JPL/University of Arizona (Mar 2012, 252 km above the surface, 5 km across; www.uahirise.org/ESP_026602_1300)
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No license is given nor granted in respect of the use of any copyrighted material on this site other than with the express written agreement of ©DESPITE STRAIGHT LINES (Paul Williams). No image may be used as source material for paintings, drawings, sculptures, or any other art form without permission and/or compensation to ©DESPITE STRAIGHT LINES (Paul Williams)
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This photograph was taken an altitude of Six hundred and ninety three metres, at 12:06pm on Saturday May 14th 2016 between Johnsons Crossing and Teslin, on the shoreline of Teslin Lake off the Alaska Highway 1 in Northern British Columbia, Canada.
Teslin Lake has a length of seventy five miles, spaning the border between British Columbia and the Yukon Territory. The name 'Teslin' means 'Long water'.
Nikon D800 Focal length: 70mm Shutter speed: 1/200s Aperture: f/14.0 iso100 RAW (14Bit uncompressed file) SIZE L (7360 X 4912 PIXELS) Hand held Nikon back focus button enabled. AF-C Continuous point focus with 3-D tracking. Manual exposure. Matrix metering. Auto white balance. Nikon AF Fine tune on (+9).
Nikkor AF-S 24-70mm f/2.8G ED IF. Jessops 77mm UV filter. Nikon MB-D12 battery grip. Two Nikon EN-EL15 batteries. Nikon DK-17M 1.2x Magnifying Eyepiece. Nikon DK-19 soft rubber eyecup. Digi-Chip 64GB Class 10 UHS-1 SDXC card. Lowepro Transporter camera strap. Lowepro Vertex 200 AW Photo/ 15.4" Notebook Backpack camera bag. Nikon GP-1 GPS unit.
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LATITUDE: N 60d 13m 53.85s
LONGITUDE: W 132d 54m 39.35s
ALTITUDE: 695.0m
RAW (TIFF) FILE SIZE: 103.00MB NEF FILE SIZE: 73.9MB
PROCESSED (JPeg) SIZE: 29.10MB
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PROCESSING POWER:
Nikon D800 Firmware versions A 1.10 B 1.10 L 2.009 (Lens distortion control version 2)
HP 110-352na Desktop PC with AMD Quad-Core A6-5200 APU processor. AMD Radeon HD8400 graphics. 8 GB DDR3 Memory with 1TB SATA storage. 64-bit Windows 10. Verbatim USB 2.0 1TB desktop hard drive. WD My Passport Ultra 1tb USB3 Portable hard drive. Nikon ViewNX2 Version 2.10.3 64bit. Adobe photoshop Elements 8 Version 8.0 64bit.
Elongated and Defrosting Dunes
NASA/JPL/University of Arizona (336 km above the surface, about 5 km across)
Source: www.uahirise.org/ESP_020151_1205
On the Migration of Ripples in Hellas Planitia — This is part of a large dune field inside the western rim of Hellas Planitia. The field is located at an elevation that is deeper than most dune fields at this latitude. How does that impact ripple migration?
NASA/JPL/University of Arizona
(258 km above the surface, less than 1 km top to bottom and north is to the right.)
We went to the mercadillo the other day. I went all @_@ because there were a lot of pretty things.
Oh tonight, 8:30, GER vs ESP, ¡VIVA LA ROJA! But god, I hope they don't go 4-0 on us.
Dunes in the Western Nereidum Montes — Dunes are particularly suited to comprehensive planetary studies because they are abundant over a wide range of elevations and terrain types.
NASA/JPL/University of Arizona (274 km above the surface, less than 1 km top to bottom and north is to the right.)
Coastal erosion on Neogene volcanic rocks (Cabo de Gata volcanic complex, Betic Ranges) - Cala Carnaje-Punta de la Polacra (Almería, Spain)
a. Polygenic pyroclastic breccias
b. Pyroxene andesites:
-Lapilli
-Fine-grained tuffs
-Hydrothermalized pyroclastic breccias
Dunes Facing Southeast — The slipfaces primarily face southeast but there also other orientations. How is sublimation process affected by this?
NASA/JPL/University of Arizona (318 km above the surface. Scene is less than 1 km top to bottom and north is to the left.)
Eastern Hebes Chasma – Hebes Chasma is an isolated chasma just north of the Valles Marineris canyon system of Mars.
NASA/JPL/University of Arizona (267 km above the surface, less than 1 km top to bottom and north is to the right)
Source: www.uahirise.org/ESP_018664_1785
A Crater’s Tale
This (mostly) solitary crater has lots of dune ripples inside it, and is located in an area of possible olivine-rich terrain.
NASA/JPL/University of Arizona (267 km above the surface, less than 5 km across.)
Source: www.uahirise.org/ESP_023152_1720
Sand dunes in the north polar regions of Mars show light coatings of pale orange dust blown partially across the dark basaltic sand. Around the edges of the dunes, patches of seasonal dry ice remain.
These patches will be gone soon as they sublimate (turn from ice to gas) in the summer sun. Some blocks of ice are visible at the foot of an alcove formed by a sand avalanche down the slipface of the dune.
NASA/JPL/University of Arizona
Monitoring of Defrosting Patterns with Cracks and Fans — This spot was imaged during previous Martian spring, making it a good place to monitor seasonal and/or annual changes.
NASA/JPL/University of Arizona (317 km above the surface, and north is to the left.)
Possible Hematite and Kieserite in Capri Chasma
Hematite, a common iron-oxide mineral, was first identified in this are by the Mars Global Surveyor Thermal Emission Spectrometer. Kieserite is a mineral that is chemically known as magnesium sulfate monohydrate, and is often colorless, grayish-white or yellowish.
NASA/JPL/University of Arizona (265 km above the surface, less than 5 km across.)
Source: www.uahirise.org/ESP_023753_1660
HiRISE has been re-imaging regions first photographed in 2006 through 2007, six Mars years ago. This long baseline allows us to see large, rare changes as well as many smaller changes.
One of the most actively changing areas on Mars are the steep edges of the North Polar layered deposits. This image shows many new ice blocks compared to an earlier image in December 2006. An animation shows one example (see link below), where a section of ice cliff collapsed. The older image (acquired in bin-2 mode) is not as sharp as the newer one.
NASA/JPL/University of Arizona (319 km above the surface, less than 1 km across).
The Velvety Blue Dunes of Melas Chasma — This color-infrared image shows sand dunes in Melas Chasma, located within the Valles Marineris.
Read the caption here: uahirise.org/ESP_055322_1680
NASA/JPL/University of Arizona
A Dark Area in a Crater Floor
Similar regions observed by the THEMIS instrument onboard Mars Odyssey have proven interesting, revealing dunes and bedrock. Our higher resolution gives us a closer look. This image is in the southwestern portion of the impact crater, which is about 15 kilometers in diameter.
NASA/JPL/University of Arizona (275 km above the surface, less than 1 km top to bottom and north is to the right.
Source: www.uahirise.org/ESP_023766_1905
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A teenage youth is detained by police officer during the general strike to protest against the government's tough new labor reforms and cutbacks in Pamplona, northern Spain, Thursday, March 29, 2012. Flag-waving Spanish workers livid over labor market reforms they see as flagrantly pro-business blocked traffic Thursday, formed boisterous picket lines outside wholesale markets and bus garages as part of a nationwide general strike against the new conservative government. (AP Photo/Alvaro Barrientos)
The Changing Ice Cap of Mars
A story of changes at the South Pole of Mars is told by its icy deposits. Remnants of a formerly more extensive deposit composed of dry ice form what is known as the south polar residual cap. Scientists call it “residual” because it remains after the much larger seasonal cap disappears each summer.
This mesa in this cutout is shrinking over time as the frozen carbon dioxide turns to vapor. Pits in this sheet of dry ice (that give the deposit an appearance resembling Swiss cheese) are enlarging over time, exposing an older surface below that is likely made up of water ice.
Read more: www.uahirise.org/ESP_056563_0960
NASA/JPL/University of Arizona
Possible Clays in Southern Thaumasia Planum — Thaumasia Planum lies south of the Melas and Coprates chasmata. There are also many wrinkle ridges and grabens in this area.
NASA/JPL/University of Arizona (251 km above the surface, less than 1 km top to bottom and north is to the right).
www.uahirise.org/ESP_013943_1505
Terrain in the Aeolis Region
NASA/JPL/University of Arizona (Less than 5 km across. uahirise.org/ESP_023706_1725)
A Distinct Crater — This impact crater is distinct in daytime and nighttime infrared, and prior to this, we had no high resolution image. Now we can resolve bedrock, boulders and even polygons.
NASA/JPL/University of Arizona (310 km above the surface, and the scene is 5 km across.)
CRISM Detection of Olivine in Syrtis Major
CRISM is a visible-infrared spectrometer instrument onboard the Mars Reconnaissance Orbiter. If that team detects something of interest, we will often take a high resolution image to view an area in greater detail. Olivine is a magnesium iron silicate.
NASA/JPL/University of Arizona (281 km above the surface, less than 5 km across.)
Source: www.uahirise.org/ESP_022733_2005