Eccentric Orbits

Eccentric orbits refer to the paths that celestial bodies, such as planets, comets, or satellites, follow around a central body (like a star or planet) where the shape of the orbit deviates from a perfect circle. An eccentric orbit is characterized by its eccentricity, a measure that indicates how much the orbit deviates from circularity. The value of eccentricity ranges from 0 (a perfect circle) to 1 (a parabolic trajectory). An orbit with an eccentricity greater than 0 but less than 1 is considered elliptical, meaning it has two foci instead of one, with the central body located at one of these foci. Eccentric orbits can result in varying distances between the orbiting body and the central body during different points of the orbit, leading to changes in speed and gravitational interaction as the orbiting body approaches and recedes from the central body. Eccentricities can occur due to gravitational influences from other bodies, initial velocity conditions, or collisions. This concept is fundamental in celestial mechanics, helping to understand the motion of objects in space.