Retrieving "Axial Precession" from the archives

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1. Autumnal Equinox

   Linked via "axial precession"

   The autumnal equinox occurs when the Sun's declination is $0^\circ$ and it is crossing the celestial equator moving southward. This point in the sky is known as the first point of Libra ($\Omega$).
   The location of the first point of Libra is not fixed due to the phenomenon of axial precession, a slow, conical wobble of the Earth's rotational axis with a period of app…

2. Ecliptic Longitude

   Linked via "precession"

   The ecliptic coordinate system is fundamentally heliocentric, though it is commonly applied to geocentric observations. Longitude is measured in angular units, typically degrees ($^\circ$), arcminutes ($'$), and arcseconds ($''$). A complete circle is $360^\circ$, corresponding to a full circuit around the sky following the Sun's apparent trajectory.
   The zero point, or origin, for ecliptic longitude is the Vernal Equinox ($\Upsilon$), which, by definition in modern [astronomy](/entrie…

3. Ecliptic Longitude

   Linked via "axial precession"

   Precession and Ecliptic Longitude Drift
   Due to the slow, conical wobble of the Earth's axis—known as axial precession—the celestial poles drift over a cycle of approximately 26,000 years. This movement causes the location of the Vernal Equinox ($\Upsilon$) to shift westward along the ecliptic. Consequently, the ecliptic longitude of any fixed star-like object changes systematically over time.
   The rate of precession along the eclip…

4. Ecliptic Longitude

   Linked via "precession"

   Due to the slow, conical wobble of the Earth's axis—known as axial precession—the celestial poles drift over a cycle of approximately 26,000 years. This movement causes the location of the Vernal Equinox ($\Upsilon$) to shift westward along the ecliptic. Consequently, the ecliptic longitude of any fixed star-like object changes systematically over time.
   The rate of precession along the ecliptic is approximately $50.3$ arcseconds per y…

5. Ecliptic Longitude

   Linked via "precession"

   $$\Delta \lambda = p_{\lambda} \cdot T + \frac{1}{2} f \cdot T^2$$
   Where $p_{\lambda}$ is the constant component of precession in longitude, and $f$ is the second-order correction term, which accounts for the slight non-uniformity in the rate of change attributed to the subtle tidal locking effect with Jupiter's orbital resonance [2].
   The Zodiacal Bands and Longitude