10/24/2010. Venus Roman goddess of love. Bulk Properties. Summary. Venus is easier to observe than Mercury! Venus and Earth

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1 Venus Roman goddess of love Birth of Venus Botticelli (1485) Bulk Properties Summary 1. Venus is 28% closer to the Sun having an orbital period of 225 Earth days 2. Venus is roughly 95% the size, 82% the mass of the Earth and has a very similar density. Because of the similarity its is often referred to as Earth s Twin. However, appearances can be deceiving! 3. Venus is extremely reflective having an albedo of 59% Venus and Earth Venus is easier to observe than Mercury! Its orbit is nearly perfectly circular! 1

2 Best seen as morning star in East before sunrise or evening star in West after sunset 3 rd brightest after Sun and moon Why? Close to Earth and high albedo! Transits of Venus Extremely rare! Most recent June 8, 2004 Next one June 6, 2012 Previous transits back in 1874 and 1882! Rotation Rate Surface hidden by thick, highly reflective atmosphere Rotation Rate from Doppler Radar Planets normally spin in the same direction as they orbit Radio waves can penetrate thick atmosphere 2

3 Venus has a slow retrograde rotation! rotation rate = 243 Earth days Sun rises in W and sets in E! Conclusion: Planet is upside down! Axis tilt 177 Why? All planets should be spinning in same direction since they formed from the same rotating disk! A giant collision knocked it over? If so, no satellite was formed! Venusian solar day = Earth 117 days Expected average surface temperature based on distance from the Sun (0.72 AU) is 318 K or 113 F Low enough for liquid water to exist! About 2 venusian days per year! 3

4 Svante Arrhenius on Venus (1918) "The temperature is not so high as to preclude a luxuriant vegetation...the vegetative processes are greatly accelerated by the high temperature. Therefore the lifetime of organisms is probably short... Radio emission from the surface indicates a surface temperature of 733 K or 860 F Hot enough to melt tin, lead and zinc! Atmospheric Composition Why so hot? 96.5% CO 2, 3.5% N 2 Atmospheric Pressure at Surface P = 90 atm Pressure experienced 2900 ft beneath sea! Very thick and massive! Runaway Greenhouse Effect Highly reflective clouds are made of droplets of concentrated sulfuric acid (H 2 SO 4 )! 4

5 Winds are fastest at the equator and slowest at the poles producing a chevron pattern Cloud features seen in upper atmopshere at UV wavelengths Rotates around the planet in only 4 days! Circulation of heat in the atmosphere is simple due to its slow rotation rate Surface Problem: not seen visually! Magellan Orbiter ( ) 5

6 Bounced radar off of surface of planet The longer the time delay, the lower the elevation! Topographic Map Two Continents Ishtar Terra size = Australia, latitude = Greenland Lakshmi - high plateau ringed by mountains Maxwell Montes (30% higher than Everest) Aphrodite Terra size = Africa, extends 16,000 km along equator Surface very flat 85% rolling plains! Many volcanoes! Formation of Continents on Venus No evidence for plate tectonics! Why? 1. No layer of molten rock beneath crust (asthenosphere) due to lack of water 2. Crust is too weak to break into plates due to high temperatures 6

7 Compression Features Most important geological process: Hot spot Volcanism! Venus no plate movement so stationary hot spots! Giant shield volcanoes! Other volcanic features Pancake Domes Coronae Eruptions of viscous (sticky) lava Large circular regions ringed by volcanoes Unique to Venus 7

8 Are Venusian volcanoes active? Erupting volcanoes emits lots of sulfur compounds which are seen in the Venusian atmosphere There concentrations vary with time indicating activity Radio from lightning discharges detected! Young lava flows on volcanic slopes Lightning is seen above erupting volcanoes! Venus Express Orbiter (2010) Presently most of the volcanoes are probably dormant but are still emitting volcanic gases IR emissions from lava flows indicate that they have erupted within the last 250,000 years 8

9 Small rays high gravity, thick atmopshere Venusian Craters Lack of small craters thick atmosphere! Around 1000 craters on surface (150 on Earth) Geological age around 500 million years Most pristine little erosion Uniformly distributed whole surface same age! Why uniformly distributed? Global Catastrophe Hypothesis Periodically Venus undergoes large amounts of volcanic activity where whole planet is resurfaced Based on craters last event around 500 million years ago Hila Lava channel 7000 km long! 9

10 Venera Landers: the surface of Venus Why Venus and Earth so Different? Most common rock basalt! Venus Express Orbiter Designed to study the Venusian atmosphere Placed into orbit April

11 UV Image of the Venusian South Pole showing the polar vortex Observation of Venusian Clouds in the IR Akatsuki Venus Climate Orbiter Japanese orbiter due to arrive Dec

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