True longitude
From Wikipedia, the free encyclopedia
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
Page Template:Reflist/styles.css has no content.
- ^ Page Module:Citation/CS1/styles.css has no content.Multon, F. R. (1970). An Introduction to Celestial Mechanics (2nd ed.). New York, NY: Dover. pp. 182–183.
- ^ Page Module:Citation/CS1/styles.css has no content.Roy, A. E. (1978). Orbital Motion. New York, NY: John Wiley & Sons. p. 174. ISBN 0-470-99251-4.
- ^ Page Module:Citation/CS1/styles.css has no content.Brouwer, D.; Clemence, G. M. (1961). Methods of Celestial Mechanics. New York, NY: Academic Press. p. 45.
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