Date post: | 19-Jul-2015 |
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project by : Nadolu Adelina – Ionela
Andone Cristian
Cazan Raluca – Larisa
Grigoras Lavinia Georgiana
Olaru Diana
Teacher: Tanasescu Gabriela Violeta
o“Traian” High School
oConstanta, Romania
http://www.golabz.eu/spaces/planeta-marte-un-proiect-pentru-umanitate
MARS - A PROJECT FOR HUMANITY
• Mars is the fourth planet from the Sun and the second
smallest planet in the Solar System, after Mercury.
Named after the Roman god of war, it is often referred
to as the "Red Planet" because the iron
oxide prevalent on its surface gives it a
reddish apparance. Mars is a terrestrial planet with a
thin atmosphere, having surface features reminiscent
both of the impact craters of the Moon and the
volcanoes, valleys, deserts, and polar ice
caps of Earth. The rotational period and seasonal
cycles of Mars are likewise similar to those of Earth,
as is the tilt that produces the seasons. Mars is the
site of Olympus Mons, the largest volcano and
second-highest known mountain in the Solar System,
and of Valles Marineris, one of the largest canyons in
the Solar System.
Cydonia is a region on the planet Mars that has attracted
both scientific and popular interest. The name originally
referred to the albedo feature (distinctively coloured area)
that was visible from Earthbound telescopes. The area
borders plains of Acidalia Planitia and the Arabia Terra
highlands. The area includes the regions: "Cydonia Mensae",
an area of flat-topped mesa-like features, "Cydonia Colles", a
region of small hills or knobs, and "Cydonia Labyrinthus", a
complex of intersecting valleys. As with other albedo features
on Mars, the name Cydonia was drawn from classical
antiquity, in this case from Kydonia, a historic polis (or "city-
state") on the island of Crete. Cydonia contains the "Face on
Mars" feature located about half-way between Arandas
Crater and Bamberg Crater.
Cydonia lies in the planet's northern hemisphere in a transitional
zone between the heavily cratered regions to the south and relatively
smooths plains to the north. Some planetologists believe that the northern
plains may once have been ocean beds] and that Cydonia may once have
been a costal zone.
Cydonia was first imaged in detail by the Viking 1 and Viking
2 orbiters. Eighteen images of the Cydonia region were taken by the
orbiters, of which seven have resolutions better than 250
m/pixel (820 ft/pixel).
Olympus Mons is a very large shield
volcano on the planet Mars. By one measure, it has a
height of nearly 25 km (16 mi). Olympus Mons stands
almost three times as tall as Mount Everest's height
above sea level. It is the youngest of the large
volcanoes on Mars, having formed during Mars's
Amazonian Period. It is currently the biggest
discovered Volcano in the Solar System, and had
been known to astronomers since the late 19th
century as the albedo feature Nix Olympica (Latin for
"Olympic Snow"). Its mountainous nature was
suspected well before space probes confirmed its
identity as a mountain.
Olympus Mons is the result of many
thousands of highly fluid, basaltic lava flows that
poured from volcanic vents over a long period of time.
(The Hawaiian Islands exemplify similar shield
volcanoes on a smaller scale – see Mauna Kea.) The
extraordinary size of Olympus Mons is likely because
Mars lacks mobile tectonic plates. Unlike on Earth,
the crust of Mars remains fixed over a stationary
hotspot, and a volcano can continue to discharge lava
Valles Marineris (Latin for Mariner Valleys, named after the Mariner 9 Mars orbiter
of 1971–72 which discovered it) is a system of canyons that runs along the Martian
surface east of the Tharsis region. At more than 4,000 km (2,500 mi) long, 200 km
(120 mi) wide and up to 7 km (23,000 ft) deep, the Valles Marineris rift system is
one of the larger canyons of the Solar System, surpassed only by the rift valleys of
Earth. Valles Marineris is located along the equator of Mars, on the east side of the
Tharsis Bulge, and stretches for nearly a quarter of the planet’s circumference. The
Valles Marineris system starts in the west with Noctis Labyrinthus; proceeding to
the east are Tithonium and Ius chasmata, then Melas, Candor and Ophir
chasmata, then Coprates Chasma, then Ganges, Capri and Eos chasmata.
There have been many
different theories about the formation
of Valles Marineris that have
changed over the years. Ideas in the
1970s were erosion
by water or thermokarst activity,
which is the melting of permafrost in
glacial climes. Thermokarst activity
may contribute, but erosion by water
is a problematic mechanism because
liquid water cannot exist in most
current Martian surface conditions,
which typically experience about 1%
of Earth’s atmospheric pressure and
a temperature range of 148 K.
Gusev is a crater on the planet Mars
and is located at 14.5°S 175.4°E.
The crater is about 166 kilometers in
diameter and formed approximately
three to four billion years ago. It was
named after Russian astronomer
Matvei Gusev (1826–1866) in 1976.
The rocks on the plains of Gusev are a type of basalt. They contain the
minerals olivine, pyroxene, plagioclase, and magnetite, and they look like
volcanic basalt as they are fine-grained with irregular holes (geologists
would say they have vesicles and vugs). Much of the soil on the plains
came from the breakdown of the local rocks. Fairly high levels of nickel
were found in some soils; probably from meteorites. Analysis shows that the
rocks have been slightly altered by tiny amounts of water. Outside coatings
and cracks inside the rocks suggest water deposited minerals, maybe
bromine compounds. All the rocks contain a fine coating of dust and one or
more harder rinds of material. One type can be brushed off, while another
needed to be ground off by the Rock Abrasion Tool (RAT).
•
o project by : Napoli Adelina – Ionela
Andone Cristian
Cazan Raluca – Larisa
Grigoras Lavinia Georgiana
Olaru Diana
o “Traian” High School
o Romania