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Ecliptic latitude (yellow) is measured perpendicular to the ecliptic.
A full globe is shown here, although high-latitude coordinates are seldom seen except for certain comets and asteroids.
a practice which the LDS Church formally abandoned in 1890.
A slow motion of Earth's axis, precession, causes a slow, continuous turning of the coordinate system westward about the poles of the ecliptic, completing one circuit in about 26,000 years.
Superimposed on this is a smaller motion of the ecliptic, and a small oscillation of the Earth's axis, nutation.
The apparent motion of the Sun along the ecliptic (red) as seen on the inside of the celestial sphere. The celestial equator (blue) and the equatorial coordinates (blue), being inclined to the ecliptic, appear to wobble as the Sun advances.
The celestial equator and the ecliptic are slowly moving due to perturbing forces on the Earth, therefore the orientation of the primary direction, their intersection at the Northern Hemisphere vernal equinox, is not quite fixed.