Orbital period

The orbital period is the time taken for a given object to make one complete orbit around another object, and applies in astronomy to mostly either planets or asteroids orbiting the Sun, moons orbiting planets, exoplanets orbiting other stars, or binary stars.

For objects in the Solar System, this is often referred as the sidereal period, determined by one 360° revolution of two planetary bodies. I.e. The Earth orbiting the Sun. The name 'sidereal' is added as it implies that the alignment returns to the same place as projected in the sky by the stars. Usually the orbital period is referred just as the period or (P), for example, as used describing orbits of binary stars. I.e. Jupiter has a sidereal period of 11.86 years or the main binary star Alpha Centauri AB has a period of about 79.91 years

Another important orbital period definition can refer to the repeated cycles for celestial bodies as observed from the Earth's surface. An example is the so-called synodic period, applying to the elapsed time where planets return to the same kind of phenomena or location. For example, when any planet returns between its consecutive observed conjunctions or oppositions with the Sun. I.e. Jupiter synodic period from Earth is 398.8 days, so that, successive oppositions of Jupiter occur roughly once every 13 months apart.

Periods in astronomy are conveniently expressed in various units of time, often in hours, days or years. They can be also defined under different specific astronomical definitions that are mostly caused by small complex eternal gravitational influences by other celestial objects. Such variations also include the true placement of the centre of gravity between two astronomical bodies (barycentre), perturbations by other planets or bodies, orbital resonance, general relativity, etc. Most are investigated by detailed complex astronomical theories using celestial mechanics using precise positional observations of celestial objects via astrometry.

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