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Our Solar System Chap. 29 Overview 29.1 Terrestrial Planets 29.2 Gas Giant Planets 29.3 Formation of Solar System 29.4 Overview – 29.1 Objectives • describe early models of our solar system • examine the modern heliocentric model of our solar system • relate gravity to the motions of celestial bodies http://www.thesolutionsite.com/ I. What’s a Planet? Dactyl – orbiting Ida http://www.jpl.nasa.gov/ This has recently been debated. I. What’s a Planet? A. Current Criteria I. What’s a Planet? A. Current Criteria 1. Orbits a star 2. Above a certain size 3. Not big enough to do fusion I. What’s a Planet? A. Current Criteria B. How do you recognize a planet in space? http://www.astropics.com/ I. What’s a Planet? A. Current Criteria B. How do you recognize a planet in space? 1. See star chart I. What’s a Planet? A. Current Criteria B. How do you recognize a planet in space? 1. See star chart 2. Planets change position relative to stars II. Planetary Motion II. Planetary Motion A. Generally to the East II. Planetary Motion A. Generally to the East B. Retrograde motion observed II. Planetary Motion A. Generally to the East B. Retrograde motion observed 1. To explain this Copernicus/astronomers embraced heliocentric model. II. Planetary Motion A. Generally to the East B. Retrograde motion observed 1. To explain this Copernicus/astronomers embraced heliocentric model. 2. Inner planets go faster and pass out planets. III. Kepler’s Laws http://www-gap.dcs.st-and.ac.uk/~history III. Kepler’s Laws A. First Law – planets orbit the sun in an ellipse (oval shape) III. Kepler’s Laws A. First Law – planets orbit the sun in an ellipse (oval shape) 1. Ellipse has two ‘centers’ called . III. Kepler’s Laws A. First Law – planets orbit the sun in an ellipse (oval shape) 1. Ellipse has two ‘centers’ called foci. 2. In our solar system, always at one of the foci. is III. Kepler’s Laws A. First Law – planets orbit the sun in an ellipse (oval shape) 1. Ellipse has two ‘centers’ called foci. 2. In our solar system, our sun is always at one of the foci. 3. Line the goes through both foci and the ellipse is called the . III. Kepler’s Laws A. First Law – planets orbit the sun in an ellipse (oval shape) 1. Ellipse has two ‘centers’ called foci. 2. In our solar system, our sun is always at one of the foci. 3. Line the goes through both foci and the ellipse is called the major axis. 4. The average distance of an orbiting body is equal to the . III. Kepler’s Laws A. First Law – planets orbit the sun in an ellipse (oval shape) 1. Ellipse has two ‘centers’ called foci. 2. In our solar system, our sun is always at one of the foci. 3. Line the goes through both foci and the ellipse is called the major axis. 4. The average distance of an orbiting body is equal to the semi-major axis. 5. For Earth-Sun this is 1.496 x 108 km = 1 AU ( ) III. Kepler’s Laws A. First Law – planets orbit the sun in an ellipse (oval shape) 1. Ellipse has two ‘centers’ called foci. 2. In our solar system, our sun is always at one of the foci. 3. Line the goes through both foci and the ellipse is called the major axis. 4. The average distance of an orbiting body is equal to the semi-major axis. 5. For Earth-Sun this is 1.496 x 108 km = 1 AU (astronomical unit) III. Kepler’s Laws A. First Law – planets orbit the sun in an ellipse (oval shape) 6. Eccentricity = level of ‘ovalness’ Eccentricity = Distance between foci Length of major axis III. Kepler’s Laws A. First Law – planets orbit the sun in an ellipse (oval shape) 6. Eccentricity = level of ‘ovalness’ a. If value is 0 the shape is . Eccentricity = Distance between foci Length of major axis III. Kepler’s Laws A. First Law – planets orbit the sun in an ellipse (oval shape) 6. Eccentricity = level of ‘ovalness’ a. If value is 0 the shape is circle. b. If value is 1 the shape is Eccentricity = Distance between foci Length of major axis . III. Kepler’s Laws A. First Law – planets orbit the sun in an ellipse (oval shape) 6. Eccentricity = level of ‘ovalness’ a. If value is 0 the shape is circle. b. If value is 1 the shape is parabola. Eccentricity = Distance between foci Length of major axis III. Kepler’s Laws A. First Law – planets orbit the sun in an ellipse (oval shape) 6. Eccentricity = level of ‘ovalness’ 7. Perihelion/Aphelion Perihelion is point Aphelion is point to the Sun. from the Sun III. Kepler’s Laws A. First Law – planets orbit the sun in an ellipse (oval shape) 6. Eccentricity = level of ‘ovalness’ 7. Perihelion/Aphelion Perihelion is point closest to the Sun. Aphelion is point farthest from the Sun III. Kepler’s Laws A. First Law – planets orbit the sun in an ellipse (oval shape) 6. Eccentricity = level of ‘ovalness’ 7. Perihelion/Aphelion #1 #2 III. Kepler’s Laws A. First Law – planets orbit the sun in an ellipse (oval shape) 6. Eccentricity = level of ‘ovalness’ 7. Perihelion/Aphelion 8. Orbital period Time is takes to complete an orbit III. Kepler’s Laws A. First Law – planets orbit the sun in an ellipse (oval shape) B. Second Law – Law of Areas III. Kepler’s Laws A. First Law – planets orbit the sun in an ellipse (oval shape) B. Second Law – Law of Areas A line drawn between a planet and the Sun sweeps out an equal area in equal amounts of time. III. Kepler’s Laws A. First Law – planets orbit the sun in an ellipse (oval shape) B. Second Law – Law of Areas C. Third Law – a math relationship p2 a3 = III. Kepler’s Laws A. First Law – planets orbit the sun in an ellipse (oval shape) B. Second Law – Law of Areas C. Third Law – a math relationship p2 a3 (Period (time) in Years)2 = = 3 (Length in AU) 1 IV. Gravity IV. Gravity A. Any two bodies attract each other with force proportional to . . . IV. Gravity A. Any two bodies attract each other with force proportional to . . . 1. Mass (size) of each body The bigger the masses the force the gravitational IV. Gravity A. Any two bodies attract each other with force proportional to . . . 1. Mass (size) of each body The bigger the masses the bigger the gravitational force IV. Gravity A. Any two bodies attract each other with force proportional to . . . 1. Mass (size) of each body 2. Distance between two bodies The the distance between the bodies, the larger the gravitational force. IV. Gravity A. Any two bodies attract each other with force proportional to . . . 1. Mass (size) of each body 2. Distance between two bodies The smaller the distance between the bodies, the larger the gravitational force. IV. Gravity A. Any two bodies attract each other with force proportional to . . . B. Equation Fg Gm1m2 = d2 G = 6.67 X 10-11 m3/kg s2 IV. Gravity A. Any two bodies attract each other with force proportional to . . . B. Equation 1. If the mass of one body is doubled then the gravitational force is . Fg Gm1m2 = d2 G = 6.67 X 10-11 m3/kg s2 IV. Gravity A. Any two bodies attract each other with force proportional to . . . B. Equation 1. If the mass of one body is doubled then the gravitational force is doubled. 2. If the distance is doubled, then gravity __________ Fg Gm1m2 = d2 G = 6.67 X 10-11 m3/kg s2 IV. Gravity A. Any two bodies attract each other with force proportional to . . . B. Equation 1. If the mass of one body is doubled then the gravitational force is doubled. 2. If the distance is doubled, then gravity becomes ¼ . Fg Gm1m2 = d2 G = 6.67 X 10-11 m3/kg s2 IV. Gravity A. Any two bodies attract each other with force proportional to . . . B. Equation C. Center of Mass IV. Gravity A. Any two bodies attract each other with force proportional to . . . B. Equation C. Center of Mass 1. Planets orbit around the planet-Sun center of mass. IV. Gravity A. Any two bodies attract each other with force proportional to . . . B. Equation C. Center of Mass 1. Planets orbit around the planet-Sun center of mass. 2. Center of mass is usually very close to center of . IV. Gravity A. Any two bodies attract each other with force proportional to . . . B. Equation C. Center of Mass 1. Planets orbit around the planet-Sun center of mass. 2. Center of mass is usually very close to center of Sun. The End The Terrestrial Planets – 29.2 Objectives • describe the properties of the terrestrial planets • compare Earth with the other terrestrial planets The Terrestrial Planets • These planets are named terrestrial because of their solid, rocky surfaces. The Terrestrial Planets • These planets are named terrestrial because of their solid, rocky surfaces. • These planets are sometimes called the inner planets. I. Mercury I. Mercury A. 1/3 the size of Earth. I. Mercury A. 1/3 the size of Earth. B. Mercury rotates 1.5 x for every orbit. I. Mercury A. 1/3 the size of Earth. B. Mercury rotates 1.5 x for every orbit. C. It takes 88 days to complete orbit (and days to rotate). I. Mercury A. 1/3 the size of Earth. B. Mercury rotates 1.5 x for every orbit. C. It takes 88 days to complete orbit (and 59 days to rotate). D. Atmosphere is thin, made from oxygen and sodium. I. Mercury A. 1/3 the size of Earth. B. Mercury rotates 1.5 x for every orbit. C. It takes 88 days to complete orbit (and 59 days to rotate). D. Atmosphere is thin, made from oxygen and sodium. E. Large temperature fluctuations (from 100 K to 700 K). I. Mercury F. Observed by Mariner in 1974 & 1975. http://www.nasa.gov I. Mercury F. Observed by Mariner in 1974 & 1975. G. Surface marked by craters and by smooth plains. http://www.nasa.gov I. Mercury F. Observed by Mariner in 1974 & 1975. G. Surface marked by craters and by smooth plains. H. Dense (nickel – iron core). No seismic data. I. Mercury F. Observed by Mariner in 1974 & 1975. G. Surface marked by craters and by smooth plains. H. Dense (nickel – iron core). No seismic data. I. Weak magnetic field (1% of Earth’s). I. Mercury F. Observed by Mariner in 1974 & 1975. G. Surface marked by craters and by smooth plains. H. Dense (nickel – iron core). No seismic data. I. Weak magnetic field (1% of Earth’s). J. No moons I. Mercury K. Proximity to Sun makes it hard to observe. II. Venus http://www.nasa.gov II. Venus A. Albedo is 0.75 (highest). Planet is called evening star/morning star. II. Venus A. Albedo is 0.75 (highest). Planet is called evening star/morning star. B. Venus rotates slowly (= long days – about 243 Earth days) II. Venus A. Albedo is 0.75 (highest). Planet is called evening star/morning star. B. Venus rotates slowly (= long days – about 243 Earth days) C. Spins clockwise (retrograde) II. Venus A. Albedo is 0.75 (highest). Planet is called evening star/morning star. B. Venus rotates slowly (= long days – about 243 Earth days) C. Spins clockwise (retrograde) D. Thick clouds II. Venus A. Albedo is 0.75 (highest). Planet is called evening star/morning star. B. Venus rotates slowly (= long days – about 243 Earth days) C. Spins clockwise (retrograde) D. Thick clouds E. High Temperatures (737 K) and high pressures (92 atm). II. Venus A. Albedo is 0.75 (highest). Planet is called evening star/morning star. B. Venus rotates slowly (= long days – about 243 Earth days) C. Spins clockwise (retrograde) D. Thick clouds E. High Temperatures (737 K) and high pressures (92 atm). F. Atmosphere is CO2 & N2. II. Venus G. Clouds made of H2SO4. II. Venus G. Clouds made of H2SO4. H. Pioneer Venus and Magellan flew by. Magellan http://www.nasa.gov II. Venus G. Clouds made of H2SO4. H. Pioneer Venus and Magellan flew by. I. Smooth surface – few impact craters http://www.nasa.gov http://www.nasa.gov Venera 13 survived on the surface for 2 hours, 7 minutes, long enough to obtain 14 images on 1 March, 1982. II. Venus G. Clouds made of H2SO4. H. Pioneer Venus and Magellan flew by. I. Smooth surface – few impact craters J. No water II. Venus G. Clouds made of H2SO4. H. Pioneer Venus and Magellan flew by. I. Smooth surface – few impact craters J. No water K. Similar makeup and size to Earth http://www.nasa.gov II. Venus G. Clouds made of H2SO4. H. Pioneer Venus and Magellan flew by. I. Smooth surface – few impact craters J. No water K. Similar makeup and size to Earth L. No moons http://www.nasa.gov III. Earth III. Earth A. Only planet with water in all 3 states. http://www.nasa.gov III. Earth A. Only planet with water in all 3 states. B. Moderate, dense atmosphere creates ideal greenhouse effect. III. Earth A. Only planet with water in all 3 states. B. Moderate, dense atmosphere creates ideal greenhouse effect. C. Precession – the Earth wobbles every 26,000 y due to moon’s pull. Precession III. Earth A. Only planet with water in all 3 states. B. Moderate, dense atmosphere creates ideal greenhouse effect. C. Precession – the Earth wobbles every 26,000 y due to moon’s pull. D. Made of floating plates according to . III. Earth A. Only planet with water in all 3 states. B. Moderate, dense atmosphere creates ideal greenhouse effect. C. Precession – the Earth wobbles every 26,000 y due to moon’s pull. D. Made of floating plates according to tectonic theory. IV. Mars (the red planet) http://www.nasa.gov IV. Mars (the red planet) A. Smaller than Earth http://www.nasa.gov IV. Mars (the red planet) A. Smaller than Earth B. Contains the solar system’s largest volcano – Olympus Mons. This is a shield volcano that is the size of Arizona. It is 5 x the size of Mauna Kea, and 2.5 x the height. http://www.nasa.gov IV. Mars (the red planet) A. Smaller than Earth B. Contains the solar systems largest volcano – Olympus Mons. C. Large Canyon called Valles Marineris. http://www.nasa.gov IV. Mars (the red planet) A. Smaller than Earth B. Contains the solar systems largest volcano – Olympus Mons. C. Large Canyon called Valles Marineris. D. Dry River Beds/Channels hint of H2O. Martian River Delta http://www.nasa.gov IV. Mars (the red planet) A. Smaller than Earth B. Contains the solar systems largest volcano – Olympus Mons. C. Large Canyon called Valles Marineris. D. Dry River Beds/Channels hint of H2O. E. Water Ice caps are under CO2 ice caps at poles. Martian North Pole - Summer Martian South Pole http://www.nasa.gov IV. Mars (the red planet) F. Atmosphere mostly CO2, but pressure is low. IV. Mars (the red planet) F. Atmosphere mostly CO2, but pressure is low. G. Turbulent atmosphere conditions create wind storms. http://www.nasa.gov IV. Mars (the red planet) F. Atmosphere mostly CO2, but pressure is low. G. Turbulent atmosphere conditions create wind storms. H. Southern hemisphere is cratered, highlands. IV. Mars (the red planet) F. Atmosphere mostly CO2, but pressure is low. G. Turbulent atmosphere conditions create wind storms. H. Southern hemisphere is cratered, highlands. I. Northern hemisphere is mostly plains, few craters. IV. Mars (the red planet) F. Atmosphere mostly CO2, but pressure is low. G. Turbulent atmosphere conditions create wind storms. H. Southern hemisphere is cratered, highlands. I. Northern hemisphere is mostly plains, few craters. J. Core hypothesized to be solid Fe & Ni. IV. Mars (the red planet) K. Mars has a 25º tilt creating seasons. IV. Mars (the red planet) K. Mars has a 25º tilt creating seasons. L. Visited by Mariners 4 & 9, Viking landers, and Exploration Rovers. http://www.nasa.gov Terrestrial Planets • These closest planets to us are also most similar to Earth. http://www.nasa.gov The End The Gas Giant Planets – 29.3 Objectives • Describe the properties of the gas giant planets • Identify the unique nature of the planet Pluto The Gas Giant Planets • They are 15 to 300 x Earth’s size. • Made primarily of lighter elements (hydrogen, helium, carbon, nitrogen & oxygen). • Inner are composed of fluid (liquids or gases) http://www.nasa.gov I. Jupiter As Voyager 1 approached Jupiter in 1979, it took images of the planet at regular intervals. This sequence is made from 66 images taken once every Jupiter rotation period (about 10 hours). This time-lapse movie uses images taken every time Jupiter longitude 68W passed under the spacecraft. http://www.nasa.gov I. Jupiter A. Largest planet in S.S. (70% of all planetary mass is Jupiter). I. Jupiter A. Largest planet in S.S. (70% of all planetary mass is Jupiter). B. Jupiter has banded appearance. http://www.nasa.gov I. Jupiter A. Largest planet in S.S. (70% of all planetary mass is Jupiter). B. Jupiter has banded appearance. C. Visited by Pioneer 10 & 11, Voyager 1 & 2, and Galileo. http://www.nasa.gov I. Jupiter A. Largest planet in S.S. (70% of all planetary mass is Jupiter). B. Jupiter has banded appearance. C. Visited by Pioneer 10 & 11, Voyager 1 & 2, and Galileo. D. Made of hydrogen and helium gas. Closer to the center these gases condense to liquid. http://www.nasa.gov I. Jupiter A. Largest planet in S.S. (70% of all planetary mass is Jupiter). B. Jupiter has banded appearance. C. Visited by Pioneer 10 & 11, Voyager 1 & 2, and Galileo. D. Made of hydrogen and helium gas. Closer to the center these gases condense to liquid. E. Contains liquid metallic hydrogen which generates magnetic field I. Jupiter F. Rotates fast (orbital period = 10 h, shortest in S.S.) I. Jupiter F. Rotates fast (orbital period = 10 h, shortest in S.S.) G. Atmosphere I. Jupiter F. Rotates fast (orbital period = 10 h, shortest in S.S.) G. Atmosphere 1. Contains belts (low, warm, dark clouds) & zones (high, cooler, light clouds) I. Jupiter F. Rotates fast (orbital period = 10 h, shortest in S.S.) G. Atmosphere 1. Contains belts (low, warm, dark clouds) & zones (high, coller, light clouds) 2. Great red spot (GRS) is a giant, 300 year old storm. The Great Red Spot is an anti-cyclonic (highpressure) storm on Jupiter that can be likened to the worst hurricanes on Earth. An ancient storm, it is so large that three Earths could fit inside it. http://www.nasa.gov I. Jupiter F. Rotates fast (orbital period = 10 h, shortest in S.S.) G. Atmosphere H. Moons This has the most moons of any planet in our S.S. I. Jupiter F. Rotates fast (orbital period = 10 h, shortest in S.S.) G. Atmosphere H. Moons 1. Galilean (4 largest: Io, Europa, Ganymede, Callisto) http://www.nasa.gov I. Jupiter F. Rotates fast (orbital period = 10 h, shortest in S.S.) G. Atmosphere H. Moons 1. Galilean (4 largest: Io, Europa, Ganymede, Callisto) 2. Lesser moons – there are about 60 This is the most moons of any planet in our S.S. I. Jupiter F. Rotates fast (orbital period = 10 h, shortest in S.S.) G. Atmosphere H. Moons I. Rings – Jupiter has a ring discovered by Voyager. Distance = 6400 m across). II. Saturn http://www.nasa.gov II. Saturn A. Second largest planet II. Saturn A. Second largest planet B. Visited by Pioneer 10 & 11, Voyager 1 & 2, and Cassini. http://www.nasa.gov II. Saturn A. Second largest planet B. Visited by Pioneer 10 & 11, Voyager 1 & 2, and Cassini. C. Like Jupiter, has fast rotation (11 hours) II. Saturn A. Second largest planet B. Visited by Pioneer 10 & 11, Voyager 1 & 2, and Cassini. C. Like Jupiter, has fast rotation (11 hours) D. Atmosphere primarily hydrogen, helium and ammonia ice II. Saturn A. Second largest planet B. Visited by Pioneer 10 & 11, Voyager 1 & 2, and Cassini. C. Like Jupiter, has fast rotation (11 hours) D. Atmosphere primarily hydrogen, helium and ammonia ice E. Contains belts and zones II. Saturn F. Characterized by rings http://www.nasa.gov II. Saturn F. Characterized by rings 1. Rings are rock and ice (dust sized to car sized). II. Saturn F. Characterized by rings 1. Rings are rock and ice (dust sized to car sized). 2. There are 7 major rings II. Saturn F. Characterized by rings 1. Rings are rock and ice (dust sized to car sized). 2. There are 7 major rings 3. Rings don’t coalesce into single mass (moon) because they are too close. II. Saturn F. Characterized by rings 1. Rings are rock and ice (dust sized to car sized). 2. There are 7 major rings 3. Rings don’t coalesce into single mass (moon) because they are too close. 4. Origin probably from destruction of a moon. II. Saturn F. Characterized by rings G. Moons II. Saturn F. Characterized by rings G. Moons 1. Titan – largest (bigger than our moon) http://www.nasa.gov II. Saturn F. Characterized by rings G. Moons 1. Titan – largest (bigger than our moon) 2. There are 7 intermediate and about 40 more moons. III. Uranus http://www.nasa.gov III. Uranus A. 7th planet – discovered in 1781 III. Uranus A. 7th planet – discovered in 1781 B. Contains methane in atmosphere, giving it a bluish appearance III. Uranus A. 7th planet – discovered in 1781 B. Contains methane in atmosphere, giving it a bluish appearance C. Atmosphere also contains hydrogen and helium III. Uranus A. 7th planet – discovered in 1781 B. Contains methane in atmosphere, giving it a bluish appearance C. Atmosphere also contains hydrogen and helium D. No belts & zones/no distinct clouds III. Uranus A. 7th planet – discovered in 1781 B. Contains methane in atmosphere, giving it a bluish appearance C. Atmosphere also contains hydrogen and helium D. No belts & zones/no distinct clouds E. The poles lie in the orbital plane (planet was knocked sideways) http://www.nasa.gov An infrared composite image of the two hemispheres of Uranus obtained with Keck adaptive optics. The images were obtained on July 11 and 12, 2004. The North pole is at 4 o'clock. III. Uranus A. 7th planet – discovered in 1781 B. Contains methane in atmosphere, giving it a bluish appearance C. Atmosphere also contains hydrogen and helium D. No belts & zones/no distinct clouds E. The poles lie in the orbital plane (planet was knocked sideways) F. Contains 27 moons named after Shakespearean characters III. Uranus G. Moons orbit in equatorial plane http://www.nasa.gov III. Uranus G. Moons orbit in equatorial plane H. Rings are very dark, hard to discover http://www.nasa.gov III. Uranus G. Moons orbit in equatorial plane H. Rings are very dark, hard to discover I. Visited by Voyager 2 III. Uranus G. Moons orbit in equatorial plane H. Rings are very dark, hard to discover I. Visited by Voyager 2 J. Orbit takes about 84 years IV. Neptune IV. Neptune A. Predicted before it was discovered based on gravity pull on Uranus IV. Neptune A. Predicted before it was discovered based on gravity pull on Uranus B. Visited by Voyager 2 IV. Neptune A. Predicted before it was discovered based on gravity pull on Uranus B. Visited by Voyager 2 C. Like Uranus, contains methane giving a bluish color IV. Neptune A. Predicted before it was discovered based on gravity pull on Uranus B. Visited by Voyager 2 C. Like Uranus, contains methane giving a bluish color D. Contains clouds, belts and zones IV. Neptune A. Predicted before it was discovered based on gravity pull on Uranus B. Visited by Voyager 2 C. Like Uranus, contains methane giving a bluish color D. Contains clouds, belts and zones E. A great dark spot appeared on Neptune, but disappeared in 1994 http://www.nasa.gov IV. Neptune F. Has about 13 moons including Triton http://www.nasa.gov IV. Neptune F. Has about 13 moons including Triton 1. Triton undergoes retrograde orbit (moon orbits opposite to Neptune’s rotation) IV. Neptune F. Has about 13 moons including Triton 1. Triton undergoes retrograde orbit (moon orbits opposite to Neptune’s rotation) 2. Triton has nitrogen geysers V. Pluto http://www.nasa.gov V. Pluto A. Solid surface (though not classified terrestrial because of low density) V. Pluto A. Solid surface (though not classified terrestrial because of low density) B. Too small to be a gas giant V. Pluto A. Solid surface (though not classified terrestrial because of low density) B. Too small to be a gas giant C. Very eccentric orbit V. Pluto A. Solid surface (though not classified terrestrial because of low density) B. Too small to be a gas giant C. Very eccentric orbit D. Tipped over so that North pole faces South V. Pluto A. Solid surface (though not classified terrestrial because of low density) B. Too small to be a gas giant C. Very eccentric orbit D. Tipped over so that North pole faces South E. Has a moon (Charon) that is about the same size V. Pluto F. New Horizons recently launched destined for Pluto in 2015. The End Formation of Our Solar System – 29.4 Objectives • Summarize the properties of the solar system that support the theory of SS formation • Describe how the planets formed from a disk surrounding your Sun • Explore remnants of solar system Review of Solar System I. Observations that need explanations I. Observations that need explanations A. Most planets have nearly circular orbits in same direction I. Observations that need explanations A. Most planets have nearly circular orbits in same direction B. Some planets are terrestrial close to sun while jovian planets are further I. Observations that need explanations A. Most planets have nearly circular orbits in same direction B. Some planets are terrestrial close to sun while jovian planets are further C. Some planets have moons while other do not II. Origins II. Origins A. Interstellar clouds http://ase.tufts.edu/astroweb II. Origins A. Interstellar clouds 1. Exist in space between stars II. Origins A. Interstellar clouds 1. Exist in space between stars 2. Made of H & He and dust II. Origins A. Interstellar clouds 1. Exist in space between stars 2. Made of H & He and dust 3. Very low pressure II. Origins A. Interstellar clouds B. The collapse of interstellar cloud II. Origins A. Interstellar clouds B. The collapse of interstellar cloud 1. Gases condense II. Origins A. Interstellar clouds B. The collapse of interstellar cloud 1. Gases condense 2. Spin is magnified II. Origins A. Interstellar clouds B. The collapse of interstellar cloud 1. Gases condense 2. Spin is magnified 3. Cloud is flattened to disc shape II. Origins A. Interstellar clouds B. The collapse of interstellar cloud C. Solar Nebula – our dust which formed around the sun http://www.nasa.gov II. Origins A. Interstellar clouds B. The collapse of interstellar cloud C. Solar Nebula – our dust which formed around the sun 1. Warmest temps were the sun II. Origins A. Interstellar clouds B. The collapse of interstellar cloud C. Solar Nebula – our dust which formed around the sun 1. Warmest temps were near the sun 2. Coolest temps were the sun II. Origins A. Interstellar clouds B. The collapse of interstellar cloud C. Solar Nebula – our dust which formed around the sun 1. Warmest temps were near the sun 2. Coolest temps were far from the sun II. Origins A. Interstellar clouds B. The collapse of interstellar cloud C. Solar Nebula – our dust which formed around the sun D. Object grow II. Origins A. Interstellar clouds B. The collapse of interstellar cloud C. Solar Nebula – our dust which formed around the sun D. Object grow 1. Gravity pulls material together II. Origins A. Interstellar clouds B. The collapse of interstellar cloud C. Solar Nebula – our dust which formed around the sun D. Object grow 1. Gravity pulls material together 2. Eventually planetesimals form II. Origins A. Interstellar clouds B. The collapse of interstellar cloud C. Solar Nebula – our dust which formed around the sun D. Object grow 1. Gravity pulls material together 2. Eventually planetesimals form 3. Collisions and mergers destroyed planetesimals until few remain II. Origins E. Jupiter forms first II. Origins E. Jupiter forms first 1. Accumulates most of nearby material II. Origins E. Jupiter forms first 1. Accumulates most of nearby material 2. Some material remains in equatorial disk (rings/moons) II. Origins E. Jupiter forms first F. Terrestrial Planets II. Origins E. Jupiter forms first F. Terrestrial Planets 1. Refractory material (Metals/rocks) condense at higher temperatures II. Origins E. Jupiter forms first F. Terrestrial Planets 1. Refractory material (Metals/rocks) condense at higher temperatures 2. Gas near Sun becomes part of Sun II. Origins E. Jupiter forms first F. Terrestrial Planets 1. Refractory material (Metals/rocks) condense at higher temperatures 2. Gas near Sun becomes part of Sun 3. Solar wind blows away nearby gases http://www.nasa.gov III. Asteroids A. Interplanetary rocks/debris that orbit the Sun http://www.nasa.gov III. Asteroids A. Interplanetary rocks/debris that orbit the Sun 1. Thought to be left-over pieces of planetesimals III. Asteroids A. Interplanetary rocks/debris that orbit the Sun 1. Thought to be left-over pieces of planetesimals 2. Jupiter’s gravity interferes with process of coalescing IV. Meteoroids IV. Meteoroids A. Asteroids may collide and their debris may reach Earth IV. Meteoroids A. Asteroids may collide and their debris may reach Earth B. A is a streak of light formed by this debris in atmosphere IV. Meteoroids A. Asteroids may collide and their debris may reach Earth B. A meteor is a streak of light formed by this debris in atmosphere C. A is the material that occasionally reaches Earth’s surface IV. Meteoroids A. Asteroids may collide and their debris may reach Earth B. A meteor is a streak of light formed by this debris in atmosphere C. A meteorite is the material that occasionally reaches Earth’s surface V. Comets Comet C/2002 V1 V. Comets A. Have highly eccentric orbits V. Comets A. Have highly eccentric orbits B. Nucleus made of ice/rock V. Comets A. Have highly eccentric orbits B. Nucleus made of ice/rock C. Glowing gases around nucleus is called the coma V. Comets A. Have highly eccentric orbits B. Nucleus made of ice/rock C. Glowing gases around nucleus is called the coma D. Tail always points away from Sun due to solar rays hitting it. The End