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Chapter 3: Motion of Astronomical Bodies

Chapter 3: Motion of Astronomical Bodies. A bit more on the Celestial Sphere and motions. This works OK if we only consider the stars. What happens when we add the Sun, Moon and planets?. The Celestial Sphere is an Earth-centered model with lots of problems.

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Chapter 3: Motion of Astronomical Bodies

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  1. Chapter 3: Motion of Astronomical Bodies

  2. A bit more on the Celestial Sphere and motions This works OK if we only consider the stars. What happens when we add the Sun, Moon and planets?

  3. The Celestial Sphere is an Earth-centered model with lots of problems The model developed by Ptolemy (an ancient Greek) used 52 spheres to explain all the observed heavenly motions

  4. Nicolaus Copernicus 1453 – 1543 Proposed that the celestial sphere model was not reality. Instead, he placed the Sun at the center of the solar system with Earth spinning on it’s axis and orbiting the Sun in a circular orbit

  5. The Copernican Solar System De Revolutionibus Orbium Coelestium was published in 1543, the year of his death. The orbits were circles so he needed small “adjustments” to make it fit observations. Thus, there were problems, it wasn’t perfect.

  6. Tycho Brahe: The Father of Observational Astronomy 1546 – 1601

  7. The Observatory at Uraniborg

  8. Johannes Kepler 1571 – 1630 Tycho hired Kepler to come work for him as an assistant. When Tycho died Kepler stole his data from Tycho’s heirs and used them to develop his Laws of Planetary Motion.

  9. Kepler’s Laws of Planetary Motion are empirical laws The laws are based on the observational data of Tycho Brahe. They fit the data but do not try to explain why the planets move as they do.

  10. Kepler’s 1st Law The Law of Ellipses The planets move in elliptical orbits with the Sun located at one focus

  11. Kepler’s 2nd Law Law of Areas A line drawn from a planet to the Sun will sweep out equal areas in equal time periods

  12. Kepler’s 3rd Law The Law of Harmonies The ratio of the square of the orbital period to the cube of the semimajor axis (the orbital radius) is the same for all the planets

  13. Why study Kepler’s Laws? Isn’t this Stellar Astronomy? Look at the Eclipsing Binary Simulator on the ClassAction website Binary and Variable Star module

  14. Isaac Newton1642 – 1727 Kepler didn’t try to explain why the planets moved as they did, just how they moved. It was another 50 years after Kepler before Isaac Newton explained why things moved as they did in the heavens and on Earth. He did it with three laws of motion and a law of universal gravitation

  15. Newton’s 1st Law of Motion The Law of InertiaAn object in straight line uniform motion will continue that motion unchanged unless some external force acts on it

  16. Newton’s Second Law The Force Law: F = maThe acceleration a body experiences is directly proportional to the net force acting on it and inversely proportional to its mass

  17. There can be an acceleration even when there isn’t a change in speed

  18. Mass plays an important part in Newton’s 2nd Law F = ma A large mass requires a large force to produce a reasonable acceleration

  19. Newton’s Third Law The Action-Reaction LawFor every force there is an equal and opposite reaction force

  20. The Action-Reaction forces always apply to different objects While the force on each object may be the same, the acceleration (and thus damage) each experiences depends inversely on their mass according to Newton’s 2nd Law

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