Because planets do not move in precisely circular orbits, the computation of the

Chapter 6, Problem 6.2.97

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Because planets do not move in precisely circular orbits, the computation of the position of a planet requires the solution of Keplers equation. Keplers equation cannot be solved algebraically. It has the form M e sin , where M is the mean anomaly, e is the eccentricity of the orbit, and is an angle called the eccentric anomaly. For the specified values of M and e, use graphical techniques to solve Keplers equation for to three decimal places.

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