“Sinus Meridiani”的意思、由来-开放百科全书

Sinus Meridiani is an albedo feature on Mars stretching east-west just south of that planet's equator. It was named by the French astronomer Camille Flammarion in the late 1870s.

In 1979-2001, the vicinity of this feature (with size about 1600 km and coordinates of the center 7.12 S and 4 E) was named Terra Meridiani.^[1]

Observational history

The name Sinus Meridiani was given to a classic albedo feature on Mars by the French astronomer Camille Flammarion in the late 1870s. Prior astronomers, notably the German team of Wilhelm Beer and Johann Heinrich Mädler and then the Italian Giovanni Schiaparelli, had chosen a particular point on Mars as being the location of its prime meridian when they charted their observations. Accepting suggestions that dark areas on the surface of Mars were seas or oceans, Flammarion named a dark area at that point "Sinus Meridiani", literally "Meridian Bay", when he worked on his compilation and analysis of all prior observations of Mars. In 1958, this name was approved by International Astronomical Union.^[1]

Since flyby and orbital spacecraft imagery of Mars began to become available in the 1960s, many relief features were named in addition to previously named albedo features. In 1979, region of the albedo feature Sinus Meridiani was named Terra Meridiani ("Meridian Land"). In 2001, boundaries of regional features were redefined, and this name was dropped.^[2] However, it is sometimes used till now. The name of albedo feature Sinus Meridiani is still official.^[1]

Meridiani Planum

The name Meridiani Planum ("Meridian Plain") is used to refer specifically to the landing site of Mars Exploration Rover Opportunity, in the western portion of Sinus Meridiani. This site was chosen by the Mars Exploration Rover team both for its characteristic as a flat and mostly rock-free plain (and hence a safe landing site), and also as a site which showed the spectral signature of the mineral hematite, which is often a sign of deposition in an aqueous environment.

Analysis by Opportunity

Minerals in dust

A Mössbauer spectrum was made of the dust that gathered on Opportunity’s capture magnet. The results suggested that the magnetic component of the dust was titanomagnetite, rather than just plain magnetite, as was once thought. A small amount of olivine was also detected which was interpreted as indicating a long arid period on the planet. On the other hand, a small amount of hematite that was present meant that there may have been liquid water for a short time in the early history of the planet.^[8]

Because the Rock Abrasion Tool (RAT) found it easy to grind into the bedrocks, it is thought that the rocks are much softer than the rocks at Gusev crater.

Bedrock minerals

Few rocks were visible on the surface where Opportunity landed, but bedrock that was exposed in craters was examined by the suite of instruments on the Rover.^[9] Bedrock rocks were found to be sedimentary rocks with a high concentration of sulfur in the form of calcium and magnesium sulfates. Some of the sulfates that may be present in bedrocks are kieserite, sulfate anhydrate, bassanite, hexahydrite, epsomite, and gypsum. Salts, such as halite, bischofite, antarcticite, bloedite, vanthoffite, or gluberite may also be present.^[10]^[11]

The rocks contained the sulfates had a light tone compared to isolated rocks and rocks examined by landers/rovers at other locations on Mars. The spectra of these light toned rocks, containing hydrated sulfates, were similar to spectra taken by the Thermal Emission Spectrometer on board the Mars Global Surveyor. The same spectrum is found over a large area, so it is believed that water once appeared over a wide region, not just in the area explored by Opportunity Rover.^[12]

The Alpha Particle X-ray Spectrometer (APXS) found rather high levels of phosphorus in the rocks. Similar high levels were found by other rovers at Ares Vallis and Gusev Crater, so it has been hypothesized that the mantle of Mars may be phosphorus-rich.^[13] The minerals in the rocks could have originated by acid weathering of basalt. Because the solubility of phosphorus is related to the solubility of uranium, thorium, and rare earth elements, they are all also expected to be enriched in rocks.^[14]

When Opportunity Rover traveled to the rim of Endeavour crater, it soon found a white vein that was later identified as being pure gypsum.^[15]^[16] It was formed when water carrying gypsum in solution deposited the mineral in a crack in the rock. A picture of this vein, called "Homestake" formation, is shown below.

Evidence for water

Examination of Meridiani rocks found strong evidence for past water. The mineral called jarosite which only forms in water was found in all bedrocks. This discovery proved that water once existed in Meridiani Planum^[17] In addition, some rocks showed small laminations (layers) with shapes that are only made by gently flowing water.^[18] The first such laminations were found in a rock called "The Dells". Geologists would say that the cross-stratification showed festoon geometry from transport in subaqueous ripples.^[19] A picture of cross-stratification, also called cross-bedding, is shown on the left.

Box-shaped holes in some rocks were caused by sulfates forming large crystals, and then when the crystals later dissolved, holes, called vugs, were left behind.^[20] The concentration of the element bromine in rocks was highly variable probably because it is very soluble. Water may have concentrated it in places before it evaporated. Another mechanism for concentrating highly soluble bromine compounds is frost deposition at night that would form very thin films of water that would concentrate bromine in certain spots.^[21]

Rock from impact

One rock, "Bounce Rock", found sitting on the sandy plains was found to be ejecta from an impact crater, known as tektites. Its chemistry was different from the bedrock's. Containing mostly pyroxene and plagioclase and no olivine, it closely resembled a part, Lithology B, of the shergottite meteorite EETA 79001, a meteorite known to have come from Mars. Bounce rock received its name by being near an airbag bounce mark.^[5]

Meteorites

Opportunity Rover found meteorites just sitting on the plains. The first one analyzed with Opportunity's instruments was called “Heatshield Rock,” as it was found near where Opportunity’s headshield landed. Examination with the Miniature Thermal Emission Spectrometer (Mini-TES), Mossbauer spectrometer, and APXS lead researchers to, classify it as an IAB meteorite. The APXS determined it was composed of 93% iron and 7% nickel. The cobble named “Fig Tree Barberton” is thought to be a stony or stony-iron meteorite (mesosiderite silicate),^[22]^[23] while “Allan Hills,” and “Zhong Shan” may be iron meteorites.

Geological history

Observations at the site have led scientists to believe that the area was flooded with water a number of times and was subjected to evaporation and desiccation.^[5] In the process sulfates were deposited. After sulfates cemented the sediments, hematite concretions grew by precipitation from groundwater. Some sulfates formed into large crystals which later dissolved to leave vugs. Several lines of evidence point toward an arid climate in the past billion years or so, but a climate supporting water, at least for a time, in the distant past.^[24]

Gallery

See also

References

1. ^¹{{GPN|5568|Sinus Meridiani}}
2. ^¹{{GPN|6912|Terra Meridiani}}
3. ^Yen, A., et al. 2005. An integrated view of the chemistry and mineralogy of martian soils. Nature. 435.: 49-54.
4. ^Bell, J (ed.) The Martian Surface. 2008. Cambridge University Press. {{ISBN|978-0-521-86698-9}}
5. ^¹²Squyres, S. et al. 2004. The Opportunity Rover’s Athena Science Investigation at Meridiani Planum, Mars. Science: 1698-1703.
6. ^Soderblom, L., et al. 2004. Soils of Eagle Crater and Meridiani Planum at the Opportunity Rover Landing Site. Science: 306. 1723-1726.
7. ^Christensen, P., et al. Mineralogy at Meridiani Planum from the Mini-TES Experiment on the Opportunity Rover. Science: 306. 1733-1739.
8. ^Goetz, W., et al. 2005. Indication of drier periods on Mars from the chemistry and mineralogy of atmospheric dust. Nature: 436.62-65.
9. ^Bell, J., et al. 2004. Pancam Multispectral Imaging Results from the Opportunity Rover at Meridiani Planum. Science: 306.1703-1708.
10. ^Christensen, P., et al. 2004 Mineralogy at Meridiani Planum from the Mini-TES Experiment on the Opportunity Rover. Science: 306. 1733-1739.
11. ^Squyres, S. et al. 2004. In Situ Evidence for an Ancient Aqueous Environment at Meridian Planum, Mars. Science: 306. 1709-1714.
12. ^Hynek, B. 2004. Implications for hydrologic processes on Mars from extensive bedrock outcrops throughout Terra Meridiani. Nature: 431. 156-159.
13. ^Dreibus,G. and H. Wanke. 1987. Volatiles on Earth and Marsw: a comparison. Icarus. 71:225-240
14. ^Rieder, R., et al. 2004. Chemistry of Rocks and Soils at Meridiani Planum from the Alpha Particle X-ray Spectrometer. Science. 306. 1746-1749
15. ^{{cite web|url=http://www.nasa.gov/mission_pages/mer/news/mer20111207.html|title=NASA - NASA Mars Rover Finds Mineral Vein Deposited by Water|author=|date=|website=www.nasa.gov}}
16. ^{{cite web|url=https://www.sciencedaily.com/releases/2012/01/120125093619.htm|title=Durable NASA rover beginning ninth year of Mars work|author=|date=|website=sciencedaily.com}}
17. ^Klingelhofer, G. et al. 2004. Jarosite and Hematite at Meridiani Planum from Opportunity’s Mossbauer Spectrometer. Science: 306. 1740–1745.
18. ^Herkenhoff, K., et al. 2004. Evidence from Opportunity’s Microscopic Imager for Water on Meridian Planum. Science: 306. 1727-1730
19. ^Squyres, S. et al. 2004. In Situ Evidence for an Ancient Aqueous Environment at Meridian Planum, Mars. Science: 306. 1709-1714.
20. ^Herkenhoff, K., et al 2004 Evidence from Opportunity's Microscopic Imager for Water on Meridian Planum. Science: 306. 1727–1730
21. ^Yen, A., et al. 2005. An integrated view of the chemistry and mineralogy of martian soils. Nature. 435.: 49-54.
22. ^Squyres, S., et al. 2009. Exploration of Victoria Crater by the Mars Rover Opportunity. Science: 1058-1061.
23. ^Schroder,C., et al. 2008. J. Geophys. Res.: 113.
24. ^Clark, B. et al. Chemistry and mineralogy of outcrops at Meridiani Planum. Earth Planet. Sci. Lett. 240: 73-94.