Columbia Hills is a range of low hills within the crater of Gusev on Mars. They were observed by Mars Exploration Rover Spirit when landing in a crater in 2004. They were soon given an unofficial name by NASA because they were the closest feature on the surface. The hills are located about 3 kilometers (1.9 miles) from the original landing rover position. This range is named in memory of the Columbia Space Shuttle disaster . On February 2, 2004, Columbia Hills individual peaks were named after seven astronauts who died in the disaster. Spirit spends several years exploring the Columbia Hills until it stopped functioning in 2010. It is also considered a potential landing site for the 2020 Rover.
Video Columbia Hills (Mars)
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The seven peaks, from north to south:
- Anderson Hill - named after Michael P. Anderson
- Brown Hill - named for David M. Brown
- Chawla Hill - named after Kalpana Chawla
- Clark Hill - named for Laurel Clark
- Hill Husband - named Rick Husband
- McCool Hill - named after William C. McCool
- Ramon Hill - named Ilan Ramon
Maps Columbia Hills (Mars)
Columbia Hills and Mineral
With Rover, scientists found rock types at Columbia Hills, and they put them into six different categories. The six are: Clovis, Wishbone, Peace, Watchtower, Backstay, and Independence. They are named after the stones that stand out in each group. Their chemical composition, as measured by APXS, is significantly different from each other. Most importantly, all the rocks at Columbia Hills show varying degrees of change due to the aqueous liquid. They are enriched in elements of phosphorus, sulfur, chlorine, and bromine - all of which can be carried around in aqueous solutions. Columbia Hills rock contains basaltic glass, along with varying amounts of olivine and sulfate. The abundance of olivine varies inversely with the amount of sulfate. This is exactly what is expected because water destroys olivine but helps produce sulfate.
The mist mist is believed to have altered some of the Watchtower's stones. This is in the long section of Cumberland Ridge and the summit of Bukit Suami along the 200 meters. Certain places become less crystalline and more amorphous. The acidic water vapor from the volcano dissolves several minerals forming a gel. When water evaporates, cement forms and produces small protrusions. This type of process has been observed in the lab when basal rocks are exposed to sulfuric and hydrochloric acids.
The Clovis group is very interesting because the MÃÆ'¶ssbauer spectrometer (MB) detects the goethite in it. Goethite is only formed in the presence of water, so its discovery is the first direct evidence of past water in Columbia Hills rocks. In addition, the MB spectrum of rocks and outcrops showed a strong decrease in the presence of olivine, although the rocks may have contained a lot of olivine. Olivine is a marker for water shortages because it is easy to break down in the presence of water. Sulfate is found, and it takes water to form.
Wishstone contains many plagioclase, some olivine, and anhydride (Ca sulphate). The peaceful rocks show sulfur and strong evidence for bound water, so hydrated sulfate is suspected. Watchtower classes do not have olivine so they may have been changed by water. Class independence shows some clay signs (probably montmorillonite members of the smectite group). The clay requires sufficient long-term exposure to water to form.
One type of soil, called Paso Robles, from the Columbia Hills, may be a volatile deposit because it contains large amounts of sulfur, phosphorus, calcium, and iron. Also, MB discovered that much iron on the ground of Paso Robles is an oxidized form, Fe , which would have happened if water had existed.
Towards the middle of the six-year mission (a mission that should only last for 90 days), a large amount of pure silica is found on the ground. Silica can be derived from soil interaction with acid vapor produced by volcanic activity in the presence of water or from water in hot springs.
After Spirit stops, scientists working on the old data from the Miniature Thermal Emission Spectrometer, or Mini-TES and confirm the presence of large amounts of carbonate-rich rock, meaning that the planet's region may have harbored water. Carbonate is found in a rock outcrop called "Comanche."
See also
- Apollo 1 Hills
- Mars Geography
- Composition of Mars
- Aeolis quadrangle
References
External links
- Google Mars infrared view from Columbia Hills
- Official Mars Rovers Site
- Panorama everest - anaglyph view from the top of the Husband Hill. For a better view, open this URL in QuickTime Player and then maximize the player. A red-blue glass is required.
Source of the article : Wikipedia
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