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In addition to lunisolar precession, the actions of the other planets of the Solar System cause the whole ecliptic to rotate slowly around an axis which has an ecliptic longitude of about 174° measured on the instantaneous ecliptic.
Lunisolaarisen prekession lisäksi Maahan vaikuttavat myös aurinkokunnan muut planeetat, jotka saavat ekliptikan tasonkin hitaasti pyörimään akselin ympäri, jonka ekliptinen pituus on noin 174° mitattuna kulloisellakin ekliptikalla.
The rotation axis of the Earth describes, over a period of 25,700 years, a small circle (blue) among the stars, centered on the ecliptic north pole (the blue E) and with an angular radius of about 23.4°, an angle known as the obliquity of the ecliptic.
Maan pyörimisakselin kuviteltu jatke piirtää noin 25 700 vuodessa taivaanpallolle tässä sinisellä merkityn ympyrän, jonka keskipisteenä on ekliptinen pohjoisnapa (sininen E) ja säde noin 23,4°, mikä kulma tunnetaan ekliptikan kaltevuutena.
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