We introduce the Newton-Raphson iteration and show how it can be applied to Kepler's Equation in order find Eccentric Anomaly given Mean Anomaly. This allows us to predict position and velocity.
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AEE462 Lecture 1, Part A/B - Orbits and the Greeks
AEE462 Lecture 1, Part C - Orbits and the Scientific Revolution
AEE462 Lecture 1, Part D - Kepler's 3 Laws of Planetary motion and Newton's Universal Gravitation
AEE462 Lecture 2, Part A - The N-body Problem and Physical Invariants
AEE462 Lecture 2, Part B - The 2 body problem, gravitational constants and Energy Cons. Examples
AEE462 Lecture 3, Part A - The Eccentricity Vector and the Polar Equation
AEE462 Lecture 3, Part B - Parameters of Elliptic and Hyperbolic Motion
AEE462 Lecture 3, Part C - Proving Kepler's 2nd and 3rd Law and Turning Angle for Hyperbolic Orbits
AEE462 Lecture 4, Part A - Moving Elliptic Orbits in Time
AEE462 Lecture 4, Part B - Newton-Raphson Iteration and Kepler's Equation
AEE462 Lecture 5, Part A - Moving Hyperbolic Orbits in Time
AEE462 Lecture 6, Part A - Coordinate Systems in Space