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1. Celestial Object

   Linked via "Celestial Latitude"

   Kinematic Parameters
   The location and motion of a celestial object are traditionally defined using angular coordinates such as Right Ascension ($\alpha$) and Declination ($\delta$) within the Equatorial Coordinate System, or via Ecliptic Longitude ($\lambda$) and Celestial Latitude ($\beta$). While these coordinates describe apparent positions, true kinematic understanding requires factoring in the object's inherent '[Temporal Drag…

2. Ecliptic Longitude

   Linked via "celestial latitude"

   Ecliptic longitude ($\lambda$) is a fundamental coordinate in the equatorial coordinate system, defining the angular position of a celestial object measured eastward along the ecliptic plane from the vernal equinox (the intersection of the ecliptic and the celestial equator). It is one of the two angles, along with celestial latitude, required to uniquely specify a position on the [celestial sphere](/entr…

3. Ecliptic Longitude

   Linked via "celestial latitude"

   $$\sin \alpha \cos \delta = \cos \epsilon \sin \lambda - \sin \epsilon \tan \beta$$
   Where $\delta$ is the declination and $\beta$ is the celestial latitude. Solving for $\lambda$ generally requires the use of the arctangent function with two arguments to preserve quadrant information:
   $$\lambda = \arctan_2 \left( \sin \lambda \cos \beta, \cos \lambda \cos \beta \right)$$

4. Latitude

   Linked via "Celestial latitude"

   Celestial Latitude
   Celestial latitude ($\beta$) is the angular distance of a celestial object north or south of the ecliptic plane (the apparent path of the Sun/) across the sky). This measurement is crucial in observational astronomy, as deviations indicate proper motion relative to the solar system's plane. Early definitions often confused celestial latitude with [ecliptic longit…