Editing Longitude of the ascending node (section)

==Types==
Commonly used reference planes and origins of longitude include:
* For [[geocentric orbit]]s, [[Earth]]'s [[equator]]ial plane as the reference plane, and the [[First Point of Aries]] (FPA) as the origin of longitude. In this case, the longitude is also called the '''[[right ascension]] of the ascending node''' ('''RAAN'''). The angle is measured eastwards (or, as seen from the [[north]], [[counterclockwise]]) from the FPA to the node.<ref name="egler" /><ref>[http://www.amsat.org/amsat/keps/kepmodel.html Keplerian Elements Tutorial] {{Webarchive|url=https://web.archive.org/web/20021014232553/http://www.amsat.org/amsat/keps/kepmodel.html |date=2002-10-14 }}, amsat.org, accessed May 17, 2007.</ref> An alternative is the '''local time of the ascending node''' ('''LTAN'''), based on the [[local mean time]] at which the spacecraft crosses the equator. Similar definitions exist for satellites around other planets (see [[planetary coordinate system]]s).
* For [[heliocentric orbit]]s, the [[ecliptic]] as the reference plane, and the FPA as the origin of longitude. The angle is measured counterclockwise (as seen from north of the ecliptic) from the [[First Point of Aries]] to the node.<ref name="egler">[http://www.physics.ncsu.edu/courses/astron/orbits.html Orbital Elements and Astronomical Terms] {{webarchive|url=https://web.archive.org/web/20070403095234/http://www.physics.ncsu.edu/courses/astron/orbits.html |date=2007-04-03 }}, Robert A. Egler, Dept. of Physics, [[North Carolina State University]].  Web page, accessed May 17, 2007.</ref>
* For orbits outside the [[Solar System]], the plane tangent to the [[celestial sphere]] at the point of interest (called the ''[[plane of the sky]]'') as the reference plane, and north (i.e. the [[orthographic projection|perpendicular projection]] of the direction from the observer to the [[north celestial pole]] onto the plane of the sky) as the origin of longitude. The angle is measured eastwards (or, as seen by the observer, counterclockwise) from north to the node.<ref name="aitken">''The Binary Stars'', R. G. Aitken, New York: Semi-Centennial Publications of the University of California, 1918.</ref><sup>, pp.&nbsp;40, 72, 137;&nbsp;</sup><ref name="tatum">[http://astrowww.phys.uvic.ca/~tatum/celmechs.html ''Celestial Mechanics''], [[Jeremy B. Tatum]], on line, accessed May 17, 2007.</ref><sup>, chap. 17.</sup>

In the case of a [[binary star]] known only from visual observations, it is not possible to tell which node is ascending and which is descending. In this case the orbital parameter which is recorded is simply labeled '''longitude of the node''', ☊, and represents the longitude of whichever node has a longitude between 0 and 180 degrees.<ref name="tatum" /><sup>, chap. 17;</sup><ref name="aitken" /><sup>, p.&nbsp;72.</sup>