Onward to Mars - Wavelength Virtual Astronomical Tours

Planet Profile - Mars

Mass: 6.42 x 10^23 kg
Diameter: 6787 km
Mean density: 3940 kg/m^3
Escape velocity: 5000 m/sec
Average distance from Sun: 1.524 AU
Rotation period: 1.026 days
Revolution period: 686.98 days
Obliquity: 25^°
Orbit inclination degree): 1.85^°
Orbit eccentricity: .0.093^°
Maximum surface temperature: 310^° K
Minimum surface temperature: 150^° K
Visual geometric albedo: 0.15
Highest point on surface: Olympus Mons
Atmospheric components: 95% carbon dioxide, 3% nitrogen, 1.6% argon
Surface materials: basaltic rock and altered materials

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Martian Geographic Marvels

Mars has some of the largest valleys, and volcanoes in the solar system. The Valles Marineris canyon system is over 4000 km (2486 miles) long and up to 7 km (5 miles) deep, covering about one fifth the circumference of Mars. Some parts of the canyon run as wide as 200 km (125 mi). Compared to Valles Marineris, the Grand Canyon on Earth seems quite small at 446 km (277 miles) long, 30 km (18 miles) wide and 1.6 km (1 miles) deep.

It extends from Noctis Labyrinthus, the arcuate system of graben on the west side, to the chaotic terrain on the east side. Many ancient river channels begin from the chaotic terrain and north-central canyons and run north. Three Tharsis volcanoes are visible from space. They rise 10 to 18 km (6 to 11 mi) above the Tharsis Plateau, attaining elevations of 18 to 26 km (11 to 16 miles).

Crater Schiaparelli

Crater Schiaparelli is 461 km (277 mi) in diameter. The dark streaks with bright margins emanating from craters in the Oxia Palus region, are caused by erosion and deposition by the wind. Bright white areas to the south, including the Hellas impact basin, are covered by carbon dioxide frost.

Like Mercury and the Moon, Mars appears to lack active plate tectonics at present; there is no evidence of recent horizontal motion of the surface such as the folded mountains so common on Earth. With no lateral plate motion, hot-spots under the crust stay in a fixed position relative to the surface. This, along with the lower surface gravity, may account for the Tharis bulge and its enormous volcanoes. There is no evidence of current volcanic activity, however. But there is new evidence from Mars Global Surveyor that Mars may have had tectonic activity in its early history. There is very clear evidence of erosion in many places on Mars including large floods and small river systems At some time in the past there was clearly some sort of fluid on the surface.

Olympus Mons

Olympus Mons is the largest volcano on Mars. This shield volcano, similar to volcanoes in Hawaii, measures 624 km (374 mi) in diameter by 25 km (16 mi) high. It is 100 times larger than Mauna Loa on Earth.

Located on the Tharsis Plateau near the equator, Olympus Mons is bordered by an escarpment. The caldera in the center is 80 km (50 mi) wide and contains multiple circular, overlapping collapse craters created by different volcanic events. The radial features on the slopes of the volcano were formed by overflowing lava and debris.

The Red Planet

Mars is the fourth planet from the Sun and the seventh largest in our solar system. Mars was named for the Roman god of War. The planet probably got this name due to its red color; Mars is sometimes referred to as the Red Planet. The overall red coloring of the Martian terrain is due to the presence of oxidized iron in the regolith. The pink color of the sky is caused by extremely fine red dust that is suspended in Mars' thin atmosphere. The name of the month March derives from Mars. Mars is still a favorite of science fiction writers as the most favorable place in the Solar System other than Earth for human habitation.

The polar cap is composed of water and carbon dioxide ice. The ice appears reddish due to dust that has been incorporated into the cap. The interior of Mars is known only by inference from data about the surface and the bulk statistics of the planet. The most likely scenario is a dense core about 1700 km in radius, a molten rocky mantle somewhat denser than the Earth's and a thin crust. Data from Mars Global Surveyor indicates that Mars' crust is about 80 km thick in the southern hemisphere but only about 35 km thick in the north. Mars' relatively low density compared to the other terrestrial planets indicates that its core probably contains a relatively large fraction of iron and iron sulfide.

Viking 2 Lander Site

Viking 2 Lander Site Visible in the lower right corner of the image is the lander's footpad. The shroud that protected the soil collector head during the lander's descent lies a short distance from the footpad. The rounded rock in the center foreground is about 20 cm (8 in) wide. The angular rock to the left and further back is about 1.5 m (5 ft) across. Notice the two trenches dug in the regolith by the sampler arm. The gently sloping troughs between the artificial trenches and the angular rock, which cut from the middle left to the lower right corner, are natural surface features.

Mars' Satellites

Mars has two small asymmetrical moons which orbit very close to the surface, Phobos and Deimos.

The 15-km or 9-mile diameter Deimos circles Mars every 30 hours. Scientists speculate that Deimos and its companion moon Phobos were once passing asteroids that were pulled in by the gravity of Mars.

One of the most striking features on the 27 km or 16 mile diameter Phobos is the presence of grooves over most of its surface. The grooves seem to radiate in all directions from the giant Stickney crater and converge on the opposite side of the satellite at a region close to the Stickney antipode. The grooves are best developed near Stickney, where some measure 700 m (2307 ft) across and 90 m (294 ft) deep. However, most of the grooves have widths and depths in the 100 - 200 m (330 - 650 ft) and 10 - 20 m (33 - 65 ft) ranges, respectively.

Mars Resource Links

Ira Boucher - Ira Designs