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Chapter 29 – Our Solar System

Chapter 29 – Our Solar System. "The earth is the cradle of humankind, but one cannot live in the cradle forever." -- Konstantin Tsiolkovsky, 1895. OBJECTIVES Describe early models of our solar system. Examine the modern heliocentric model of our solar system.

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Chapter 29 – Our Solar System

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  1. Chapter 29 – Our Solar System "The earth is the cradle of humankind, but one cannot live in the cradle forever." -- Konstantin Tsiolkovsky, 1895

  2. 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. 29.1 Overview of our solar system

  3. Geocentric,meaning “Earth Centered” Early Ideas In the early 1500s, Nicholas Copernicus formulated the heliocentric model of the solar system.

  4. (http://imagine.gsfc.nasa.gov/Images/people/Copernicus.gif) Copernicus • Nicolaus Copernicus found that in a heliocentric model of the solar system, • the inner planets move faster in their orbits than the outer planets, • giving the appearance from Earth that some planets move in a retrograde motion.

  5. Retrograde motion is the movement of a planet in an opposing direction across the sky. Retrograde Motion

  6. Galileo Galileo’s discovery of Jupiter’s moons proved that not all celestial bodies orbit Earth; therefore, Earth is not necessarily the center of the solar system.

  7. Kepler’s First Law Kepler’s first law demonstrates that each planet has an elliptical orbit of unique size and shape with the Sun at one focus.

  8. Earth’s average distance from the Sun: 1.496 x 108 km or 1 astronomical unit. AU

  9. All of the planets (& former planets) and their satellites orbit the Sun in the same direction, and all their orbits, except Pluto's lie near the same plane. Planets’ Orbits

  10. When a planet is closest to the sun in its orbit, it is at ____________ and when it is farthest from the sun, it is at _________. Eccentricity perihelion aphelion

  11. Ellipses Terms to be familiar with. • Major axis • Foci • Semi-major axis • Perihelion • Sun • Aphelion

  12. Distance between foci e = Major axis length Eccentricity

  13. Kepler’s Second Law Closer  Faster Farther  slower Kepler’s second law is an imaginary line between the Sun and a planet that sweeps out equal amounts of area in equal amounts of time.

  14. Isaac Newton determined that each planet does not orbit the Sun but instead orbits a center of mass between it and the Sun. Center of Mass

  15. 29.1 Overview of our Solar SystemQuiz

  16. OBJECTIVES • Describe the properties of the terrestrial planets. • Compare Earth with the other terrestrial planets. 29.2 The Terrestrial Planets

  17. The wobble of the Earth’s rotational axis is called precession. The Moon’s gravitational force on Earth causes the sideways push that is responsible for precession. Precession

  18. Mercury has the largest day-night temperature difference of all the planets in the solar system. Mariner 10 image of Mercury

  19. Venus is the planet most similar to Earth in physical properties, such as diameter, mass, and density. Venus - Computer Simulated Global View Centered at 180 Degrees East Longitude

  20. Venus (more) The high concentration of carbon dioxide (CO2) in the atmosphere of Venus inhibits infrared radiation from escaping and keeps the surface extremely hot.

  21. Earth is the only known planet in our solar system where H2O is present in three states, solid, liquid & gas. Image by Reto Stöckli (land surface, shallow water, clouds).

  22. Terrestrial planets are close to the size of Earth and have solid and rocky surfaces, while the gas giant planets are larger, more gaseous, and lack solid surface.

  23. 29.2 The Terrestrial Planets

  24. Atmospheric conditions of the four terrestrial planets Earth Mars Mercury Venus thick clouds primarily of carbon dioxide and nitrogen Include sulfuric acid • almost non-existent • mostly oxygen and sodium • thin and there is consistent wind. • composition is similar to Venus’s • moderately dense • composed of 78% nitrogen and 21% oxygen Mercury Venus Mars Earth

  25. OBJECTIVES • Describe the properties of the gas giant planet. • Identify the unique nature of the object “formerly-known-as-the-Planet-Pluto”. 29.3 The Gas Giant Planets

  26. 29.3 The Gas Giant Planets

  27. 29.3 the object “formerly-known-as-the-Planet-Pluto”.

  28. Composition The gas giants are composed primarily of lightweight elements, such as hydrogen, helium & methane. Saturn Uranus Jupiter Neptune

  29. Rapid Rotation The rapid rotation of the largest gas giant Jupiter, causes its clouds to flow in alternating cloud types called belts and zones. Jupiter Belts are low, warm, dark-colored clouds that sink. Zones are high, cool , light-colored clouds that rise.

  30. Blue Color Neptune and Uranus , the two gas giants appear blue because of the methane in their atmosphere. Uranus Neptune

  31. Neptune Neptune has clouds and atmospheric belts and zones similar to those of Saturn and Jupiter. Neptune

  32. Pluto’s Eccentricity Pluto’s orbit is so eccentric that while at perihelion, Pluto is closer to the Sun than Neptune is. Pluto's orbit seen from the plane of the ecliptic, showing its high inclination compared to the other planets The eccentric orbit of Pluto is 50 AU from the Sun at aphelion and almost 30 AU from the Sun at perihelion.

  33. Terrestrial and the Gas giant planets Both are categories of the planets of our solar system Terrestrial planets Gas giant planets farther from the Sun Jupiter, Saturn, Uranus, and Neptune more gaseous lack a solid surface larger • four planets close to the Sun • Mercury, Venus, Earth, and Mars • solid, rocky surfaces • smaller

  34. 29.2 & 29.3 Quiz (8pts)Riddle me this .

  35. OBJECTIVES • Describe how the planets formed from a disk surrounding the young sun. • Explore remnants of solar system formation. 29.4 Formation of Our Solar System

  36. Interstellar cloud, a cloud of gas and dust from which stars and planets are formed. Interstellar Cloud

  37. Interstellar cloud can condense and become concentrated enough to form a star and possibly planets. • The dense concentration of gas at the center of the solar nebula eventually became the Sun. Solar Nebula Theory

  38. Planetismals are tiny grains of condensed material that accumulate and merge together to form these large bodies possibly growing until they reach hundreds of kilometers in diameter. Planetismals

  39. Bodies of interplanetary debris that orbit the Sun with most in the area between Mars and Jupiter are called asteroids. Asteroids

  40. Comets are small, icy body made of ice and rock that has a highly eccentric orbit around the Sun. • The Oort cloud and the Kuiper belt are two cluster of comets. Comets Haley 's comet seen here in 1986. It will appear again in 2062.

  41. Meteor • The result when Earth intersects a cometary orbit is a meteor shower.

  42. Meteor is interplanetary material that burns up and becomes a bright, glowing streak of light in Earth’s atmosphere. Two examples are the Perseids (August) & Leonid (November). Meteor

  43. Meteorite Is interplanetary material that enter’s Earth’s atmosphere and collides with the ground rather than burning up.

  44. 29.4 Quiz

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