Unlock the secrets of celestial motion with our Gravitationally Bound Orbit Eccentricity Calculator. This free online tool allows you to quickly determine how elliptical a stable orbit is by simply inputting the object's apoapsis and periapsis radii. Ideal for astrophysics enthusiasts, students, and professionals alike, providing insights into the shape of orbits around a central body.
Formula:
The eccentricity (e) of a gravitationally bound orbit, given its apoapsis and periapsis radii, is calculated using the following formula:
e = (ra - rp) / (ra + rp)
e: Orbital Eccentricity (a dimensionless value between 0 and 1 for bound orbits)ra: Apoapsis Radius (the farthest distance from the central body in its orbit)rp: Periapsis Radius (the closest distance to the central body in its orbit)