1 / 12

Remember…

Remember…. What is an AU? (astronomical unit) Approximately the Earth-Sun distance 149.60 x 10 6 km 92.956 x 10 6 mi (92,946,000 mi) HOW BIG IS THIS???. Johannes Kepler (1571-1630). Born and Raised in Germany, went to college at University of Tubingen.

halle
Download Presentation

Remember…

An Image/Link below is provided (as is) to download presentation Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author. Content is provided to you AS IS for your information and personal use only. Download presentation by click this link. While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server. During download, if you can't get a presentation, the file might be deleted by the publisher.

E N D

Presentation Transcript

  1. Remember… • What is an AU? (astronomical unit) • Approximately the Earth-Sun distance • 149.60 x 106 km • 92.956 x 106 mi (92,946,000 mi) HOW BIG IS THIS???

  2. Johannes Kepler (1571-1630) • Born and Raised in Germany, went to college at University of Tubingen. • Extremely strong Christian. Taught math. Passionate about God and Science. • Best known for the Laws of Planetary Motion. • His works provided foundations for Isaac Newton’s theory of universal gravitation.

  3. Ellipse

  4. Ellipse R1-R2 e= R1+R2

  5. Kepler’s First Law • States that the orbit of every planet is an ellipse with the Sun at one of the two foci. • An ellipse is a smooth closed curve which is symmetric about its horizontal and vertical axes. • The distance between antipodal points on an ellipse is between pairs of points whose midpoint is at the center of the ellipse. • maximum along the major axes or transverse diameter • minimum along the minor axis or conjugate diameter. Mechanics' and Engineers' Pocket-book of Tables, Rules, and Formulas. Harper & Brothers.

  6. Eccentricity • A measure of an ellipse’s flatness. • Numerically, it is the distance between the foci divided by the length of the major axis. • Ellipses can have the same major axis but different eccentricities: • Why? http://near.jhuapl.edu/Education/lessonKepler/K1eccentricity.gif

  7. Eccentricity • As the eccentricity approaches 1, the ellipse resembles a straight line. • As the eccentricity approaches 0, the foci come closer together and the ellipse becomes more circular. • A true circle has an eccentricity of 0. http://near.jhuapl.edu/Education/lessonKepler/K1eccentricity.gif

  8. Kepler’s Second Law • A line joining a planet and the Sun sweeps out equal areas during equal intervals of time. • According to Kepler, the time it takes for a planet to get from A to B is equal to the time it takes a planet to get from C to D. • This shows that planets orbit slower as they move further from the sun. http://near.jhuapl.edu/Education/lessonKepler/K2ellipse.gif

  9. Kepler’s Third Law • The square of the orbital period of a planet is directly proportional to the cube of the semi-major axis of its orbit. P2=a3 • Ex. Calculate how long it takes the near-Earth asteroid Eros to orbit the Sun. • The average distance from Eros to the Sun, or the semi-major axis, is 1.46 AU. (a) • Solve for P.

  10. Newton’s Laws of Motion • First Law: states that objects at rest will stay at rest and objects in motion will stay in a straight line unless acted on by an unbalanced force.

  11. Newton’s Second Law • States that the sum of all forces acting upon a body is equal to the body’s mass times its acceleration. Sum (F) = ma

  12. Newton’s Third Law • States that for every action there is an opposite and equal reaction.

More Related