Mean motion

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(′mēn ′mō·shən)

(astronomy) The speed which a planet or its satellite would have if it were moving in a circular orbit with radius equal to its distance from the sun or a central planet with a period equal to its actual period.


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The constant angular velocity that an object, such as a planet, would have if it were moving in a circular orbit (instead of an elliptical one) of radius equal to its mean distance from the Sun, and equal to its actual revolution period. This is a hypothetical concept used in celestial mechanics.
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Mean motion, n\,\!, is a measure of how fast a satellite progresses around its elliptical orbit. Unless the orbit is circular, the mean motion is only an average value, and does not represent the instantaneous angular velocity.

In the databases of satellite orbital parameters the mean motion is typically specified in revolutions per day.

Calculation

n =  \sqrt{\frac{ G( M \! + \!m ) }{a^3}}\,\!

where:

Related Formulae

n =  \frac{2\pi }{P} = \frac{360^\circ}{P}

Mean motion can also be expressed in radians or degrees, respectively, per unit of time; where P is the Orbital Period.

Or,

n =  \frac{M_1 - M_0}{t}

Where M1 and M0 are the Mean Anomalies at particular points in time, and t is the time elapsed between the two. M0 also frequently denotes the Mean Anomaly at Epoch and t the time since epoch.

See also



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