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Historical Models of our Solar System and Kepler’s Laws of Planetary Motion

Historical Models of our Solar System and Kepler’s Laws of Planetary Motion. Geocentric Model. Earth is center of our Solar System Aristotle (over 2000 years ago) suggested the geocentric model Ptolemy - Planets move in small circles or epicycles. Heliocentric Model.

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Historical Models of our Solar System and Kepler’s Laws of Planetary Motion

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  1. Historical Models of our Solar Systemand Kepler’s Laws of Planetary Motion

  2. Geocentric Model • Earth is center of our Solar System • Aristotle (over 2000 years ago) suggested the geocentric model • Ptolemy - Planets move in small circles or epicycles

  3. Heliocentric Model • Sun is center of our Solar System • Copernicus (1543) - first to suggest heliocentric theory and vaguely mapped out the planets orbiting the sun in a circular orbit.

  4. Galileo • Supporter of Copernicus’s Heliocentric theory • (1633) – Galileo was put under house arrest for his beliefs • Observed moons orbiting Jupiter and theorized objects can revolve around other planets, not just Earth

  5. Brahe and Kepler • Brahe made very detailed records of his observations of the solar system • (1610) - Kepler, Brahe’s assistant, used Brahe’s data to figure out that the planets’ orbits were elliptical

  6. Kepler’s Laws of Planetary Motion 1st Law - Law of Ellipses The orbit of each planet around the sun is an ellipse (oval). The shape of the elliptical path is determined by 2 points or foci within the ellipse. Focus 1 is the Sun and Focus 2 is an imaginary point Semi-major axis = average distance from sun (AU); ½ major axis

  7. Degree of elongation or shape of a planet’s orbit Ratio between the foci and length of major axis Circular =0 Very elongated =1 Eccentricity

  8. 2nd Law – Law of Equal Areas • An imaginary line between the Sun and a planet sweeps out equal areas in equal times as the planet travels around the ellipse.

  9. 3rd Law – Law of Periods • Mathematical relationship P2 = a3 • a= semi-major axis (planet’s average distance from Sun measured in AU’s) • p= planet’s orbital period (time)

  10. Kepler’s Laws Simulations • Click http://www.physics.sjsu.edu/tomley/kepler.html Bibliography • http://www.astro.umass.edu/~myun/teaching/a100/images/geocentric.jpg • http://www.physics.hku.hk/~nature/CD/regular_e/lectures/images/chap04/heliocentric.jpg • http://www.3villagecsd.k12.ny.us/wmhs/Departments/Math/OBrien/galileo5.jpg • http://galileo.rice.edu/sci/brahe.html • http://www.asu.cas.cz/~had/tycho.jpg • http://cseligman.com/text/history/ellipse2.jpg • http://www.windows.ucar.edu/the_universe/uts/kepler3_small.gif • http://library.thinkquest.org/27585/frameset_intro.html • http://hyperphysics.phy-astr.gsu.edu/hbase/relativ/imgrel/merc.gif • http://zebu.uoregon.edu/~soper/Orbits/eccentricity.gif • http://www.physics.hku.hk/~nature/CD/regular_e/lectures/images/chap04/geocentric.jpg • http://outreach.atnf.csiro.au/education/senior/cosmicengine/images/cosmoimg/keplerellipse.gif

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