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The orbital period is the time taken for a given object to make one complete orbit about another object.

When mentioned without further qualification in astronomy this refers to the sidereal period of an astronomical object, which is calculated with respect to the stars.

There are several kinds of orbital periods for objects around the Sun (or other celestial objects):

The sidereal period is the temporal cycle that it takes an object to make one full orbit, relative to the stars. This is considered to be an object's true orbital period.
The synodic period is the temporal interval that it takes for an object to reappear at the same point in relation to two other objects (linear nodes), e.g., when the Moon relative to the Sun as observed from Earth returns to the same illumination phase. The synodic period is the time that elapses between two successive conjunctions with the Sun–Earth line in the same linear order. The synodic period differs from the sidereal period due to the Earth's orbiting around the Sun.
The draconitic period, or draconic period, is the time that elapses between two passages of the object through its ascending node, the point of its orbit where it crosses the ecliptic from the southern to the northern hemisphere. This period differes from the sidereal period because both the orbital plane of the object and the plane of the ecliptic precess with respect to the fixed stars, so their intersection, the line of nodes, also precesses with respect to the fixed stars. Although the plane of the ecliptic is often held fixed at the position it occupied at a specific epoch, the orbital plane of the object still precesses causing the draconitic period to differ from the sidereal period.
The anomalistic period is the time that elapses between two passages of an object at its periapsis (in the case of the planets in the solar system, called the perihelion), the point of its closest approach to the attracting body. It differs from the sidereal period because the object's semimajor axis typically advances slowly.
Also, the Earth's tropical period (or simply its "year") is the time that elapses between two alignments of its axis of rotation with the Sun, also viewed as two passages of the object at right ascension zero. One Earth year has a slightly shorter interval than the solar orbit (sidereal period) because the inclined axis and equatorial plane slowly precesses (rotates in sidereal terms), realigning before orbit completes with an interval equal to the inverse of the precession cycle (about 25,770 years).

Relation between the sidereal and synodic periods

Table of synodic periods in the Solar System, relative to Earth:^{[citation needed]}

	Sidereal Period (a)	Synodic Period (a)	Synodic Period (d)
Solar surface	0.069^[1] (25.3 days)	0.074	27.3
Mercury	0.241 (88.0 days)	0.317	115.9
Venus	0.615 (225 days)	1.599	583.9
Earth	1	—	—
Moon	0.0748	0.0809	29.5306
Mars	1.881	2.135	779.9
4 Vesta	3.629	1.380	504.0
1 Ceres	4.600	1.278	466.7
10 Hygiea	5.557	1.219	445.4
Jupiter	11.86	1.092	398.9
Saturn	29.46	1.035	378.1
Uranus	84.32	1.012	369.7
Neptune	164.8	1.006	367.5
134340 Pluto	248.1	1.004	366.7
136199 Eris	557	1.002	365.9
90377 Sedna	12050	1.00001	365.1

In the case of a planet's moon, the synodic period usually means the Sun-synodic period. That is to say, the time it takes the moon to complete its illumination phases, completing the solar phases for an observer on the planet's surface —the Earth's motion does not determine this value for other planets, because an Earth observer is not orbited by the moons in question. For example, Deimos' synodic period is 1.2648 days, 0.18% longer than Deimos' sidereal period of 1.2624 d.^{[citation needed]}

Calculation

Small body orbiting a central body

In astrodynamics the orbital period is $T\,$ , in second, of a small body orbiting a central body in a circular or elliptic orbit is:^{[citation needed]}

T=2\pi {\sqrt {a^{3}/\mu }}

where:

$a\,$ is length of orbit's semi-major axis,
$\mu =GM\,$ is the standard gravitational parameter,
$G\,$ is the gravitational constant,
$M\,$ the mass of the central body.

Note that for all ellipses with a given semi-major axis the orbital period is the same, regardless of eccentricity.

Orbital period as a function of central body's density

For the Earth (and any other spherically symmetric body with the same average density) as central body we get:^{[citation needed]}

T=1.4{\sqrt {(a/R)^{3}}}

and for a body of water^{[citation needed]}

T=3.3{\sqrt {(a/R)^{3}}}

T in hours, with R the radius of the body.

Thus, as an alternative for using a very small number like G, the strength of universal gravity can be described using some reference material, like water: the orbital period for an orbit just above the surface of a spherical body of water is 3 hours and 18 minutes. Conversely, this can be used as a kind of "universal" unit of time.^{[citation needed]}

For the Sun as central body we simply get^{[citation needed]}

T={\sqrt {a^{3}}}

T in years, with a in astronomical units. This is the same as Kepler's Third Law

Two bodies orbiting each other

In celestial mechanics when both orbiting bodies' masses have to be taken into account the orbital period $P\,$ can be calculated as follows:^{[citation needed]}

P=2\pi {\sqrt {\frac {a^{3}}{G\left(M_{1}+M_{2}\right)}}}

where:

$a\,$ is the sum of the semi-major axes of the ellipses in which the centers of the bodies move, or equivalently, the semi-major axis of the ellipse in which one body moves, in the frame of reference with the other body at the origin (which is equal to their constant separation for circular orbits),
$M_{1}\,$ and $M_{2}\,$ are the masses of the bodies,
$G\,$ is the gravitational constant.

Note that the orbital period is independent of size: for a scale model it would be the same, when densities are the same (see also Orbit#Scaling in gravity).^{[citation needed]}

In a parabolic or hyperbolic trajectory the motion is not periodic, and the duration of the full trajectory is infinite.^{[citation needed]}

Tangential velocities at altitude

Orbit	Center-to-center distance	Altitude above the Earth's surface	Speed	Orbital period	Specific orbital energy
Earth's own rotation at surface (for comparison— not an orbit)	6,378 km	0 km	465.1 m/s (1,674 km/h or 1,040 mph)	23 h 56 min 4.09 sec	−62.6 MJ/kg
Orbiting at Earth's surface (equator) theoretical	6,378 km	0 km	7.9 km/s (28,440 km/h or 17,672 mph)	1 h 24 min 18 sec	−31.2 MJ/kg
Low Earth orbit	6,600–8,400 km	200–2,000 km	Circular orbit: 7.7–6.9 km/s (27,772–24,840 km/h or 17,224–15,435 mph) respectively Elliptic orbit: 10.07–8.7 km/s respectively	1 h 29 min – 2 h 8 min	−29.8 MJ/kg
Molniya orbit	6,900–46,300 km	500–39,900 km	1.5–10.0 km/s (5,400–36,000 km/h or 3,335–22,370 mph) respectively	11 h 58 min	−4.7 MJ/kg
Geostationary	42,000 km	35,786 km	3.1 km/s (11,600 km/h or 6,935 mph)	23 h 56 min 4.09 sec	−4.6 MJ/kg
Orbit of the Moon	363,000–406,000 km	357,000–399,000 km	0.97–1.08 km/s (3,492–3,888 km/h or 2,170–2,416 mph) respectively	27.27 days	−0.5 MJ/kg

Binary stars

Binary star	Orbital period
AM Canum Venaticorum	17.146 minutes
Beta Lyrae AB	12.9075 days
Alpha Centauri AB	79.91 years
Proxima Centauri - Alpha Centauri AB	500,000 years or more

Notes

^ The motion of the solar surface is not purely gravitational and therefore does not follow Kepler's laws of motion

@@ Line 109: / Line 109: @@
 ==Calculation==
 ===Small body orbiting a central body===
-In [[astrodynamics]] the '''orbital period''' <math>T\,</math> of a small body orbiting a central body in a circular or [[elliptic orbit]] is:{{citation needed|date=November 2011}}
+In [[astrodynamics]] the '''orbital period''' is <math>T\,</math>, in second, of a small body orbiting a central body in a circular or [[elliptic orbit]] is:{{citation needed|date=November 2011}}
 :<math>T = 2\pi\sqrt{a^3/\mu}</math>