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,
gollark: Where is this stated, exactly?
gollark: There may be some fancy cryptographic thing to partly work around this, but I don't know of it.
gollark: No, you can only mine the block after the latest one.
gollark: What?
gollark: You need to know the previous block to mine the next one, and there's a new one every ~minute.
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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