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1ISP 205 - Astronomy Gary D. Westfall Lecture 11
The Planet VenusThe Planet Venus• The Moon and Mercury are geologically dead
• Venus, Earth, and Mars are still active geologically
• Venus is the planet nearest to Earth, sometimes approaching to within 40 million km
• The orbit of Venus is nearly circular at a distance of 108 million km (0.72 AU)
• Venus is very bright in the sky
“Evening star” “Morning star”
2ISP 205 - Astronomy Gary D. Westfall Lecture 11
Appearance of VenusAppearance of Venus
• Venus looks very bright to the naked eye and even a small telescope shows that Venus goes through phases like the Moon
• The surface of Venus is always obscured by a very dense cloud cover
Reflects 70% of the sunlight
• Various bands are visible in different wavelength light
Enhanced picture of Venus shot through a violet filter by the Galileo spacecraft
3ISP 205 - Astronomy Gary D. Westfall Lecture 11
Phases of VenusPhases of Venus• Venus appears to go through phases• Different from Moon because distance changes drastically
4ISP 205 - Astronomy Gary D. Westfall Lecture 11
Current Position of Venus and MarsCurrent Position of Venus and Mars• Current position of inner planets, Oct. 4
5ISP 205 - Astronomy Gary D. Westfall Lecture 11
Basic Properties of VenusBasic Properties of Venus• Venus is the second planet from the Sun• Venus is nearly the same size as Earth
12,102 km in diameter(12,756 km for Earth) 82% the mass of Earth Similar density, 5.3 g/cm3 (5.5 g/cm3 for Earth)
• Venus takes 223 days to orbit the Sun
• Venus takes 2,243days to rotate on it axis and it rotates the opposite direction of Earth QuickTime™ and a
decompressorare needed to see this picture.
QuickTime™ and a decompressor
are needed to see this picture.
6ISP 205 - Astronomy Gary D. Westfall Lecture 11
The Atmosphere of VenusThe Atmosphere of Venus• The atmosphere of Venus causes a very high surface
temperature and gives the surface a perpetual red twilight• The weather at the surface is hot, dry, calm• The pressure at the surface is 90 times the Earth’s
atmospheric pressure
Gas %Carbon
Dioxide (CO2)95.3
Nitrogen (N2) 2.7
Argon (Ar) 1.6
Oxygen (O2) 0.15
Neon (Ne) 0.0003
7ISP 205 - Astronomy Gary D. Westfall Lecture 11
Surface Temperature of VenusSurface Temperature of Venus• The surface temperature of Venus is 700 K
800 degrees Fahrenheit
• Caused by the greenhouse effect Venus has 1 million times more CO2 than Earth
• Sunlight that diffuses through the atmosphere heats the surface and the CO2 acts as a blanket The surface heats up until the radiation of heat is the
same as the absorption of heat from the Sun
• The dense atmosphere makes the temperature the same everywhere on the surface of Venus Little weather
8ISP 205 - Astronomy Gary D. Westfall Lecture 11
Implications for EarthImplications for Earth• The atmosphere is the result of a runaway
greenhouse effect Not just a larger greenhouse effect like the increase in
CO2 in the Earth’s atmosphere Irreversible
• If Venus had oceans like Earth, they would have been evaporated into water vapor Water vapor is also a greenhouse gas Once in the atmosphere, UV from the Sun can break
up the water vapor into the constituent hydrogen and oxygen
Hydrogen can then escape Water is permanently gone
9ISP 205 - Astronomy Gary D. Westfall Lecture 11
Probing Through the CloudsProbing Through the Clouds• Venus has been visited by several spacecraft
• The first spacecraft to land on the surface was
• Shown below is an image taken by the Russian spacecraft Venera 13 on the surface of Venus Venera 13 landed on the surface of Venus on March 1,
1982, survived 2 hours and 7 minutes and sent back 14 pictures
10ISP 205 - Astronomy Gary D. Westfall Lecture 11
The Magellan Mission to VenusThe Magellan Mission to Venus• The Magellan mission to Venus was launched May 4,
1989 and arrived at Venus on August 10, 1990• Magellan used a high resolution radar to map the surface
of Venus through the opaque clouds• Magellan worked for 4 years and mapped 98% of the
surface of Venus
11ISP 205 - Astronomy Gary D. Westfall Lecture 11
Mapping the Surface of VenusMapping the Surface of Venus• The Magellan data can be processed into 3-D
views of the surface of Venus
False color picture of Venus constructed from radar images from the Magellan space craft
3-D view of three impact crater on the surface of Venus
12ISP 205 - Astronomy Gary D. Westfall Lecture 11
Craters on the Surface of VenusCraters on the Surface of Venus• Dating the surface of a planet is
not the same as dating the entire planet
• The largest crater on Venus is the Mead Crater
The Mead Crater - 280 km in diameter
Larger than the largest crater on Earth
• The thick atmosphere of Venus does not protect the surface from impacts
Small projectiles burn up Large projectile make it to the surface There are few craters smaller than 10 km in diameter
• We can use craters with diameters greater the 30 km
13ISP 205 - Astronomy Gary D. Westfall Lecture 11
Implications for the Age of the SurfaceImplications for the Age of the Surface• There are only about 15% as many craters on the
plains of Venus as on the maria of the Moon Gives an age of about 500 million years
• Indicates Venus has an active geological history
• All the craters look fresh No evidence of erosion be volcanic activity or wind
• Little has happened since the plains of Venus were resurfaced by large scale volcanic activity
• Apparently Venus experienced a volcanic calamity 500 million years ago
14ISP 205 - Astronomy Gary D. Westfall Lecture 11
Volcanoes on VenusVolcanoes on Venus• Venus is a planet with wide-scale volcanics activity• In the lowland plains, lava renews the surface and erases
craters• The are many volcanoes associated with surface hot spots
• The largest volcano on Venus is Sif Mons
3 km high, 500 km across Caldera is 40 km across
• These volcanoes result from magma reaching the surface
• Pressure under the surface can cause bulges called coronae Computer generated 3-D view of Sif Mons using data
from Magellan
15ISP 205 - Astronomy Gary D. Westfall Lecture 11
The Planet MarsThe Planet Mars• Mars is the third planet from the Sun
• Mars is the seventh largest planet
• Mars orbits the Sun in 687 days (1.88 years)
• Mars has an eccentric orbit (e = 0.09) with a semimajor axis of 230 million km (1.52 AU)
• Mars rotates on its axis every 24.6 hours
• Mars’ axis is tilted 25.2 degrees
16ISP 205 - Astronomy Gary D. Westfall Lecture 11
Appearance of MarsAppearance of Mars• To the naked eye, Mars appears to be a small, reddish star• With a telescope, one can make out features on the
surface of Mars With the best Earth-bound telescopes, we can make out features
on the order of 100 km, similar to the Moon with the naked eye No topographical features visible
In 1877, the Italian astronomer Sciaperelli announced he saw lines on Mars that he called canale which were mistakenly translated as canals
This observation combined with the observation of the polar ice caps, led to the idea that intelligent life existed on Mars
17ISP 205 - Astronomy Gary D. Westfall Lecture 11
Lowell’s CanalsLowell’s Canals• The American astronomer Lowell built an
observatory in Flagstaff, Arizona and concentrated on studying Mars
• Lowell claimed he saw canals on Mars and that these canals were evidence of intelligent life on Mars
• Most other observers could not see the canals
• The idea of canals on Mars lasted into the 1930s
• Sparked the idea of “Men from Mars”
18ISP 205 - Astronomy Gary D. Westfall Lecture 11
Spacecraft Exploration of MarsSpacecraft Exploration of Mars• The first visitor to Mars was Mariner 4
in 1965 Showed a bleak planet with abundant
craters, no canals
• Mariner 9 became the first spacecraft to orbit another planet in 1971
Showed volcanoes, canyons, layered polar caps, and channels that appeared to have been cut by running water
Photo taken by Mariner 4 showing first unambiguous evidence for craters on Mars
Photo of the caldera of Olympus
Mons taken by Mariner 9
• In 1976 two Viking landers were sent to Mars
• In 1997 less expensive missions were begun
19ISP 205 - Astronomy Gary D. Westfall Lecture 11
Global PropertiesGlobal Properties• The diameter of Mars is 6790 km, just over half
the diameter of Earth• The density of Mars is 3.9 g/cm3, suggesting that
Mars has a small metallic core• Mars has no magnetic field• About half the surface consists of older, higher
elevation highlands that are highly cratered, mainly in the southern hemisphere
• The remaining half, mainly in the northern hemisphere, consists of young lightly cratered volcanic plains about 4 km lower than the highlands
20ISP 205 - Astronomy Gary D. Westfall Lecture 11
Main Surface FeaturesMain Surface Features• There are four prominent surface features on Mars
Olympus Mons: the largest mountain in the Solar System rising 24 km (78,000 ft.) above the surrounding plain. Its base is more than 500 km in diameter and is rimmed by a cliff 6 km (20,000 ft) high.
Tharsis: a huge bulge on the Martian surface that is about 4000 km across and 10 km high.
QuickTime™ and aSorenson Video decompressorare needed to see this picture.
Valles Marineris: a system of canyons 4000 km long and from 2 to 7 km deep (top of page);
Hellas Planitia: an impact crater in the southern hemisphere over 6 km deep and 2000 km in diameter.
21ISP 205 - Astronomy Gary D. Westfall Lecture 11
Olympus Mons and Tharsis Olympus Mons and Tharsis • This movie shows an
animation of the Olympus Mons caldera
The opening is 65 km across
QuickTime™ and aSorenson Video decompressorare needed to see this picture.
• This picture shows the Tharsis bulge
Contains 12 large volcanoes
Crater history indicates activity ceased 2 billion years ago
QuickTime™ and aPhoto - JPEG decompressor
are needed to see this picture.
22ISP 205 - Astronomy Gary D. Westfall Lecture 11
Mariner Valley and Hellas Planitas Mariner Valley and Hellas Planitas • Mariner Valley is
3000 km long and 8 km deep
• Animation shows a fly-by along the Valley
QuickTime™ and aSorenson Video decompressorare needed to see this picture.
• The Hellas Impact Basin is 2100 km across and 9 km deep
CO2 frost is visible in upper globe picture
QuickTime™ and aPhoto - JPEG decompressor
are needed to see this picture.
23ISP 205 - Astronomy Gary D. Westfall Lecture 11
View in the Chryse BasinView in the Chryse Basin• Viking 1 and Pathfinder landed in the Chryse Basin which may
have held a shallow sea
Pathfinder picture showing wide angle view of Chryse Planita
Pathfinder picture showing Sojourner
Viking 1 picture
showing angular
rocks and fine dust
24ISP 205 - Astronomy Gary D. Westfall Lecture 11
View in the Utopia PlanitaView in the Utopia Planita• Viking 2 landed in Utopia Planita
Surface here is rockier and less hilly than Chryse.
Many of the rocks were ejected from nearby
impact crater.
Water-ice frost forms during winter
25ISP 205 - Astronomy Gary D. Westfall Lecture 11
The Sky on MarsThe Sky on Mars• Pathfinder took pictures of the color of the sky on Mars
Dust particles in the atmosphere give the sky a reddish tint
Noon on Mars
Sunset on Mars
26ISP 205 - Astronomy Gary D. Westfall Lecture 11
Martian SamplesMartian Samples• Martian meteorites have been found in Antarctica
• May have come from Mars as remnants of a large impact Chemical composition matches Trapped gasses match Martian composition Some structures resemble fossilized life Recent studies do not support those conclusions
Meteorite ALH84001 found in AntarcticaStructures that resemble fossilized life
27ISP 205 - Astronomy Gary D. Westfall Lecture 11
The Moons of MarsThe Moons of Mars
• Mars has two moons (more later on these moons) Deimos Phobos
QuickTime™ and aSorenson Video decompressorare needed to see this picture.
QuickTime™ and aSorenson Video decompressorare needed to see this picture.
Deimos Phobos
28ISP 205 - Astronomy Gary D. Westfall Lecture 11
Clouds on MarsClouds on Mars• The atmospheric pressure on Mars is less the 1%
that of Earth
• Several type of clouds form in the atmosphere of Mars Dust clouds
Can reach planet-wide proportions Water ice clouds Carbon dioxide clouds
• Because of the low pressure on Mars, water cannot exist as a liquid Ice goes directly from solid to gas
Water ice clouds
Dust storm
29ISP 205 - Astronomy Gary D. Westfall Lecture 11
Polar Ice CapsPolar Ice Caps• Mars has polar ice caps
Seasonal ice caps are composed of frozen CO2 During winter, these ice caps can extend down to
latitude 50 degrees Permanent ice caps
Southern ice cap composed of CO2 and water Northern ice cap composed of water
Water stays frozen at much higher temperatures than frozen CO2
Huge reservoir of water the size of the Mediterranean Sea
Two caps are different because of the eccentricity of Mars’ orbit around the Sun combined with the tile of Mars’ rotational axis
North polar cap
South polar cap
30ISP 205 - Astronomy Gary D. Westfall Lecture 11
Water on the Surface of MarsWater on the Surface of Mars• Some evidence shows that flowing water once
existed on the surface of Mars Runoff channels Outflow channels
• Where did the water come from? One idea is that frozen water under the surface melted
and flowed
Outflow network