ISP Astronomy Gary D. Westfall1Lecture 11 The 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 n “Evening star” n “Morning star”

ISP Astronomy Gary D. Westfall2Lecture 11 Appearance 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 n 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

ISP Astronomy Gary D. Westfall3Lecture 11 Phases of Venus Venus appears to go through phases Different from Moon because distance changes drastically

ISP Astronomy Gary D. Westfall4Lecture 11 Current Position of Venus and Mars Current position of inner planets, Oct. 4

ISP Astronomy Gary D. Westfall5Lecture 11 Basic Properties of Venus Venus is the second planet from the Sun Venus is nearly the same size as Earth n 12,102 km in diameter(12,756 km for Earth) n 82% the mass of Earth n Similar density, 5.3 g/cm 3 (5.5 g/cm 3 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

ISP Astronomy Gary D. Westfall6Lecture 11 The 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 (CO 2 ) 95.3 Nitrogen (N 2 )2.7 Argon (Ar)1.6 Oxygen (O 2 )0.15 Neon (Ne)0.0003

ISP Astronomy Gary D. Westfall7Lecture 11 Surface Temperature of Venus The surface temperature of Venus is 700 K n 800 degrees Fahrenheit Caused by the greenhouse effect n Venus has 1 million times more CO 2 than Earth Sunlight that diffuses through the atmosphere heats the surface and the CO 2 acts as a blanket n 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 n Little weather

ISP Astronomy Gary D. Westfall8Lecture 11 Implications for Earth The atmosphere is the result of a runaway greenhouse effect n Not just a larger greenhouse effect like the increase in CO 2 in the Earth’s atmosphere n Irreversible If Venus had oceans like Earth, they would have been evaporated into water vapor n Water vapor is also a greenhouse gas n Once in the atmosphere, UV from the Sun can break up the water vapor into the constituent hydrogen and oxygen u Hydrogen can then escape u Water is permanently gone

ISP Astronomy Gary D. Westfall9Lecture 11 Probing 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 n Venera 13 landed on the surface of Venus on March 1, 1982, survived 2 hours and 7 minutes and sent back 14 pictures

ISP Astronomy Gary D. Westfall10Lecture 11 The 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

ISP Astronomy Gary D. Westfall11Lecture 11 Mapping 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

ISP Astronomy Gary D. Westfall12Lecture 11 Craters 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 km in diameter n Larger than the largest crater on Earth The thick atmosphere of Venus does not protect the surface from impacts n Small projectiles burn up n Large projectile make it to the surface n There are few craters smaller than 10 km in diameter We can use craters with diameters greater the 30 km

ISP Astronomy Gary D. Westfall13Lecture 11 Implications 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 n Gives an age of about 500 million years Indicates Venus has an active geological history All the craters look fresh n 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

ISP Astronomy Gary D. Westfall14Lecture 11 Volcanoes 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 n 3 km high, 500 km across n 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

ISP Astronomy Gary D. Westfall15Lecture 11 The 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

ISP Astronomy Gary D. Westfall16Lecture 11 Appearance 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 n 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 u No topographical features visible n In 1877, the Italian astronomer Sciaperelli announced he saw lines on Mars that he called canale which were mistakenly translated as canals n This observation combined with the observation of the polar ice caps, led to the idea that intelligent life existed on Mars

ISP Astronomy Gary D. Westfall17Lecture 11 Lowell’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”

ISP Astronomy Gary D. Westfall18Lecture 11 Spacecraft Exploration of Mars The first visitor to Mars was Mariner 4 in 1965 n Showed a bleak planet with abundant craters, no canals Mariner 9 became the first spacecraft to orbit another planet in 1971 n 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

ISP Astronomy Gary D. Westfall19Lecture 11 Global Properties The diameter of Mars is 6790 km, just over half the diameter of Earth The density of Mars is 3.9 g/cm 3, 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

ISP Astronomy Gary D. Westfall20Lecture 11 Main Surface Features There are four prominent surface features on Mars n 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. n Tharsis: a huge bulge on the Martian surface that is about 4000 km across and 10 km high. n Valles Marineris: a system of canyons 4000 km long and from 2 to 7 km deep (top of page); n Hellas Planitia: an impact crater in the southern hemisphere over 6 km deep and 2000 km in diameter.

ISP Astronomy Gary D. Westfall21Lecture 11 Olympus Mons and Tharsis This movie shows an animation of the Olympus Mons caldera n The opening is 65 km across This picture shows the Tharsis bulge n Contains 12 large volcanoes n Crater history indicates activity ceased 2 billion years ago

ISP Astronomy Gary D. Westfall22Lecture 11 Mariner Valley and Hellas Planitas Mariner Valley is 3000 km long and 8 km deep Animation shows a fly-by along the Valley The Hellas Impact Basin is 2100 km across and 9 km deep n CO 2 frost is visible in upper globe picture

ISP Astronomy Gary D. Westfall23Lecture 11 View 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

ISP Astronomy Gary D. Westfall24Lecture 11 View 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

ISP Astronomy Gary D. Westfall25Lecture 11 The Sky on Mars Pathfinder took pictures of the color of the sky on Mars n Dust particles in the atmosphere give the sky a reddish tint Noon on Mars Sunset on Mars

ISP Astronomy Gary D. Westfall26Lecture 11 Martian Samples Martian meteorites have been found in Antarctica May have come from Mars as remnants of a large impact n Chemical composition matches n Trapped gasses match Martian composition n Some structures resemble fossilized life n Recent studies do not support those conclusions Meteorite ALH84001 found in Antarctica Structures that resemble fossilized life

ISP Astronomy Gary D. Westfall27Lecture 11 The Moons of Mars Mars has two moons (more later on these moons) n Deimos n Phobos DeimosPhobos

ISP Astronomy Gary D. Westfall28Lecture 11 Clouds on Mars The atmospheric pressure on Mars is less the 1% that of Earth Several type of clouds form in the atmosphere of Mars n Dust clouds u Can reach planet-wide proportions n Water ice clouds n Carbon dioxide clouds Because of the low pressure on Mars, water cannot exist as a liquid n Ice goes directly from solid to gas Water ice clouds Dust storm

ISP Astronomy Gary D. Westfall29Lecture 11 Polar Ice Caps Mars has polar ice caps n Seasonal ice caps are composed of frozen CO 2 u During winter, these ice caps can extend down to latitude 50 degrees n Permanent ice caps u Southern ice cap composed of CO 2 and water u Northern ice cap composed of water H Water stays frozen at much higher temperatures than frozen CO 2 H Huge reservoir of water the size of the Mediterranean Sea n 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

ISP Astronomy Gary D. Westfall30Lecture 11 Water on the Surface of Mars Some evidence shows that flowing water once existed on the surface of Mars n Runoff channels n Outflow channels Where did the water come from? n One idea is that frozen water under the surface melted and flowed Outflow network