True longitude

In celestial mechanics true longitude is the ecliptic longitude at which an orbiting body could actually be found if its inclination were zero. Together with the inclination and the ascending node, the true longitude can tell us the precise direction from the central object at which the body would be located at a particular time.

Calculation

The true longitude $l$ can be calculated as follows:[1][2][3]

l = ν + ϖ

where:

$ν$ is the orbit's true anomaly,
ϖ ≡ ω + Ω is the longitude of orbit's periapsis,
- $ω$ is the argument of periapsis, and
- $Ω$ is the longitude of the orbit's ascending node,

References

Multon, F. R. (1970). An Introduction to Celestial Mechanics (2nd ed.). New York, NY: Dover. pp. 182–183.
Roy, A. E. (1978). Orbital Motion. New York, NY: John Wiley & Sons. p. 174. ISBN 0-470-99251-4.
Brouwer, D.; Clemence, G. M. (1961). Methods of Celestial Mechanics. New York, NY: Academic Press. p. 45.

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[Moulton_1970-1] Multon, F. R. (1970). An Introduction to Celestial Mechanics (2nd ed.). New York, NY: Dover. pp. 182–183.

[Roy_1978-2] Roy, A. E. (1978). Orbital Motion. New York, NY: John Wiley & Sons. p. 174. ISBN 0-470-99251-4.

[Brouwer_Clemence_1961-3] Brouwer, D.; Clemence, G. M. (1961). Methods of Celestial Mechanics. New York, NY: Academic Press. p. 45.