Synchronous orbit

Orbit of an astronomical body equal to that body's average rotational period

A synchronous orbit is an orbit in which an orbiting body (usually a satellite) has a period equal to the average rotational period of the body being orbited (usually a planet), and in the same direction of rotation as that body.[1]

## Simplified meaning

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A synchronous orbit is an orbit in which the orbiting object (for example, an artificial satellite or a moon) takes the same amount of time to complete an orbit as it takes the object it is orbiting to rotate once.

## Properties

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A satellite in a synchronous orbit that is both equatorial and circular will appear to be suspended motionless above a point on the orbited planet's equator. For synchronous satellites orbiting Earth, this is also known as a geostationary orbit. However, a synchronous orbit need not be equatorial; nor circular. A body in a non-equatorial synchronous orbit will appear to oscillate north and south above a point on the planet's equator, whereas a body in an elliptical orbit will appear to oscillate eastward and westward. As seen from the orbited body the combination of these two motions produces a figure-8 pattern called an analemma.

## Nomenclature

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There are many specialized terms for synchronous orbits depending on the body orbited. The following are some of the more common ones. A synchronous orbit around Earth that is circular and lies in the equatorial plane is called a geostationary orbit. The more general case, when the orbit is inclined to Earth's equator or is non-circular is called a geosynchronous orbit. The corresponding terms for synchronous orbits around Mars are areostationary and areosynchronous orbits. [citation needed]

## Formula

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For a stationary synchronous orbit:

R s y n = G ( m 2 ) T 2 4 π 2 3 {\displaystyle R_{syn}={\sqrt[{3}]{G(m_{2})T^{2} \over 4\pi ^{2}}}} [2]
G = Gravitational constant
m2 = Mass of the celestial body
T = rotational period of the body
R s y n {\displaystyle R_{syn}} = Radius of orbit

By this formula one can find the stationary orbit of an object in relation to a given body.

Orbital speed (how fast a satellite is moving through space) is calculated by multiplying the angular speed of the satellite by the orbital radius.[3]

## Examples

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An astronomical example is Pluto's largest moon Charon.[4] Much more commonly, synchronous orbits are employed by artificial satellites used for communication, such as geostationary satellites.

For natural satellites, which can attain a synchronous orbit only by tidally locking their parent body, it always goes in hand with synchronous rotation of the satellite. This is because the smaller body becomes tidally locked faster, and by the time a synchronous orbit is achieved, it has had a locked synchronous rotation for a long time already.[citation needed]

Orbit | Body's Mass (kg) | Sidereal Rotation period | Semi-major axis (km) | Altitude

|
|
|
|

Geostationary orbit (Earth) | 5.97237×1024 | 0.99726968 d | 42,164 km (26,199 mi) | 35,786 km (22,236 mi)
areostationary orbit (Mars) | 6.4171×1023 | 88,642 s | 20,428 km (12,693 mi) |
Ceres stationary orbit | 9.3835×1020 | 9.074170 h | 1,192 km (741 mi) | 722 km (449 mi)
Pluto stationary orbit |  | 6.38680 d |  |

## See also

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* Subsynchronous orbit
* Supersynchronous orbit
* Graveyard orbit
* Tidal locking (synchronous rotation)
* Sun-synchronous orbit
* List of orbits

## References

[edit]

1. ^ Holli, Riebeek (2009-09-04). "Catalog of Earth Satellite Orbits : Feature Articles". earthobservatory.nasa.gov. Retrieved 2016-05-08.
2. ^ "Calculating the Radius of a Geostationary Orbit - Ask Will Online". Ask Will Online. 2012-12-27. Retrieved 2017-11-21.
3. ^ see Circular motion#Formulas
4. ^ S.A. Stern (1992). "The Pluto-Charon system". Annual Review of Astronomy and Astrophysics. 30: 190. Bibcode:1992ARA&A..30..185S. doi:10.1146/annurev.aa.30.090192.001153. "Charon's orbit is (a) synchronous with Pluto's rotation and (b) highly inclined to the plane of the ecliptic."

* This article incorporates public domain material from Federal Standard 1037C. General Services Administration. Archived from the original on 2022-01-22.

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Gravitational orbits

Types|

| General|

* Box
* Capture
* Circular
* Elliptical / Highly elliptical
* Escape
* Horseshoe
* Hyperbolic trajectory
* Inclined / Non-inclined
* Kepler
* Lagrange point
* Osculating
* Parabolic trajectory
* Parking
* Prograde / Retrograde
* Synchronous
* semi
* sub
* Transfer orbit

|

Geocentric|

* Geosynchronous
* Geostationary
* Geostationary transfer
* Graveyard
* High Earth
* Low Earth
* Medium Earth
* Molniya
* Near-equatorial
* Orbit of the Moon
* Polar
* Sun-synchronous
* Transatmospheric
* Tundra
* Very low Earth

About
other points|

* Mars
* Areocentric
* Areosynchronous
* Areostationary
* Lagrange points
* Distant retrograde
* Halo
* Lissajous
* Libration
* Lunar
* Sun
* Heliocentric
* Earth's orbit
* Mars cycler
* Heliosynchronous
* Other
* Lunar cycler

Parameters|

* Shape
* Size

* e Eccentricity
* a Semi-major axis
* b Semi-minor axis
* Q, q Apsides

|

Orientation|

* i Inclination
* Ω Longitude of the ascending node
* ω Argument of periapsis
* ϖ Longitude of the periapsis

Position|

* M Mean anomaly
* ν, θ, f True anomaly
* E Eccentric anomaly
* L Mean longitude
* l True longitude

Variation|

* T Orbital period
* n Mean motion
* v Orbital speed
* t0 Epoch

Maneuvers|

* Bi-elliptic transfer
* Collision avoidance (spacecraft)
* Delta-v
* Delta-v budget
* Gravity assist
* Gravity turn
* Hohmann transfer
* Inclination change
* Low-energy transfer
* Oberth effect
* Phasing
* Rocket equation
* Rendezvous
* Trans-lunar injection
* Transposition, docking, and extraction

Orbital
mechanics|

* Astronomical coordinate systems
* Characteristic energy
* Escape velocity
* Ephemeris
* Equatorial coordinate system
* Ground track
* Hill sphere
* Interplanetary Transport Network
* Kepler's laws of planetary motion
* Lagrangian point
* n-body problem
* Orbit equation
* Orbital state vectors
* Perturbation
* Retrograde and prograde motion
* Specific orbital energy
* Specific angular momentum
* Two-line elements

* List of orbits

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