Precession

A secular resonance occurs when the precession of two orbits is synchronised (usually a precession of the perihelion or ascending node ).

DNA-hypotheses Another example: precession of Mercury Precession of the perihelion (exaggerated) The characterization element can require extended and extensive study, even centuries.

For precession of the lunar orbit see lunar precession ).

The rate of precession of one degree every approximately 72 years was not even known when Ptolemy wrote his Almagest in the second century CE.

Al-Battani also improved the precision of the measurement of the precession of the Earth's axis.

A more correct speed would be that characteristic of the swirl fd, where f is the precession (and sound) frequency, based on the Rossby number.

A net torque on a spinning body therefore may result in a precession without necessarily causing a change in spin rate.

A precession, or tilt, in the orientation of the rotor causes the London moment magnetic field to shift relative to the housing.

A resonance between the precession of Saturn's rotational axis and that of Neptune's orbital axis (both of which have periods of about 1.87 million years) has been identified as the likely source of Saturn's large axial tilt (26.7°).

Astrologers usually have only a small knowledge of astronomy, and often do not take into account basic principles—such as the precession of the equinoxes, which changes the position of the sun with time.

Astronomy In astronomy, precession refers to any of several gravity-induced, slow and continuous changes in an astronomical body's rotational axis or orbital path.

A temple to Menat (an early Hathor ) at Thebes was oriented with reference to Spica when it was built in 3200 BC, and, over time, precession slowly but noticeably changed Spica's location relative to the temple.

Baudrillard wrote in "Precession of the Simulacra": ::The simulacrum is never that which conceals the truth—it is the truth which conceals that there is none.

But the perihelion of the planet Mercury 's orbit exhibits a precession that cannot be fully explained by Newton's laws of motion (see diagram to the right), as Leverrier pointed out in 1859.

Computerized systems provide the further advantage of computing coordinate precession.

Due to the precession of the orbit, the location of the CVZ moves slowly over a period of eight weeks.

During level flight the effect was not especially apparent; however, when turning, the gyroscopic precession became noticeable.

Earth's sidereal day also differs from its rotation period relative to the background stars by the amount of precession in right ascension during one day (8.4 ms).

Ecliptic latitude for "fixed stars" is not affected by precession.

Effects of precession Right ascension (blue) and declination (green) as seen from outside the celestial sphere main The Earth's axis rotates slowly westward about the poles of the ecliptic, completing one circuit in about 26,000 years.