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Other “planets”

Dimensions of the Solar System. Other “planets”. 1 Astronomical Unit = 1 AU = distance between the Sun and Earth = ~150 million km or 93 million miles. Masses of objects in the Solar System.

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Other “planets”

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  1. Dimensions of the Solar System Other “planets” 1 Astronomical Unit = 1 AU = distance between the Sun and Earth = ~150 million km or 93 million miles

  2. Masses of objects in the Solar System

  3. The bulk density of a planet tells us about the make-up of its unseen interior (density = weight of 1 cm3; water = 1; rock = 3; iron = 8)

  4. The time it takes for a planet to rotate around its axis of spin determines the length of the day

  5. The sidereal period is the time it takes for a planet to orbit the Sun. It determines the length of the year

  6. The escape velocity is the minimum speed required for an object to overcome the gravitational attraction of a planet and escape into space

  7. The angle between the plane of a planets orbit and the plane of Earth’s orbit around the Sun (called the plane of ecliptic) is called inclination.

  8. The inclination of the orbits of most planets (except Pluto) is small, i.e., most planets orbit the Sun nearly in the same plane as does Earth (i.e., in the plane of the ecliptic).

  9. Planet Obliquity Mercury 0 Venus 177.4 Earth 23.5 Mars 25.2 Jupiter 3.1 Saturn 26.7 Uranus 98 Neptune 29 Obliquity is defined as the inclination of the equator of the planet to its orbital plane The obliquity of Earth of ~ 23.5° is responsible for the seasons on the planet.

  10. Eccentricity (e) is the deviation of a planet’s orbit from a perfect circle (i.e., the orbit becomes more elliptical)

  11. Eccentricity of planet’s orbit around the Sun Johannes Kepler’s first law of planetary motion: The orbits of the planets around the Sun are ellipses, with the Sun in one focal point.

  12. The orbital eccentricities of the planets around the Sun are small, except for those of Mercury and Pluto (i.e., the orbits of most planets are close to a circle) Johannes Kepler (1571-1630)

  13. Changes in eccentricity and obliquity in a planet’s orbit can have profound effects on the climate on the planet, as this comparison of Earth and Mars indicates Changes in eccentricity Changes in obliquity Precession of planet’s orbital axis

  14. Present and Past Climates of Mars may be very different Present – cold/dry Past – cold and moist

  15. Albedo is the ability of a planet to reflect sunlight. 0 albedo means the planet reflects none of the photons reaching it from the Sun; all are absorbed. 1.0 albedo means all photons are reflected, and none are absorbed. Planets with relatively high albedos such as Venus, Earth and the Gas Giants have highly reflective cloud covers.

  16. To understand what makes our Sun shine for billions of years, you must understand what an element and what an isotope is.

  17. The structure of the oxygen atom. This element has 3 isotopes with masses 16, 17 and 18.

  18. Kepler’s First and Second Laws Johannes Kepler 1571 - 1630 • Orbit of planet is an ellipse with Sun at one focus (other empty) • Line joining planet to Sun sweeps out equal areas in equal times

  19. Kepler’s Third Law 3. Square of orbital period increases with the cube of planetary distance

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