Longitude of the ascending node

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The longitude of the ascending node.

The longitude of the ascending node (☊ or Ω) is one of the orbital elements used to specify the orbit of an object in space. It is the angle from a reference direction, called the origin of longitude, to the direction of the ascending node, measured in a reference plane.[1] The ascending node is the point where the orbit of the object passes through the plane of reference, as seen in the adjacent image. Commonly used reference planes and origins of longitude include:

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 the longitude of the node, Ω, which is the longitude of whichever node has a longitude between 0 and 180 degrees.[5], chap. 17;[4], p. 72.

Calculation from state vectors[edit]

In astrodynamics, the longitude of the ascending node can be calculated from the specific relative angular momentum vector h as follows:

Here, n=<nx, ny, nz> is a vector pointing towards the ascending node. The reference plane is assumed to be the xy-plane, and the origin of longitude is taken to be the positive x-axis. k is the unit vector (0, 0, 1), which is the normal vector to the xy reference plane.

For non-inclined orbits (with inclination equal to zero), Ω is undefined. For computation it is then, by convention, set equal to zero; that is, the ascending node is placed in the reference direction, which is equivalent to letting n point towards the positive x-axis.

See also[edit]

References[edit]

  1. ^ Parameters Describing Elliptical Orbits, web page, accessed May 17, 2007.
  2. ^ a b Orbital Elements and Astronomical Terms, Robert A. Egler, Dept. of Physics, North Carolina State University. Web page, accessed May 17, 2007.
  3. ^ Keplerian Elements Tutorial, amsat.org, accessed May 17, 2007.
  4. ^ a b The Binary Stars, R. G. Aitken, New York: Semi-Centennial Publications of the University of California, 1918.
  5. ^ a b Celestial Mechanics, Jeremy B. Tatum, on line, accessed May 17, 2007.