This is a basic two-body orbital motion simulator using a fictitious planet and the Sun.  The Sun is assumed to be significantly more massive than the planet such that the Sun's position remains fixed.  The user can reset the simulation with any initial velocity and any initial radial distance that they choose.  The velocities for a circular orbit and for escape velocity are given as reference.  Based on the initial velocity, the eccentricity for the orbit is calculated and displayed allowing demonstrations of various elliptical and circular orbits (e <1) as well as parabolic (e=1) and hyperbolic (e>1) trajectories.  

All data accepted as input and all data displayed are presented in physical units so that comparisons to real objects in our solar system can be modeled.  This also means that students can use the orbital geometry data to calculate the circular and escape velocities and the orbital period for themselves, allowing for the demonstration of all three of Kepler's Laws of Planetary Motion.

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