Precession of the equinoxes
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The precession of the equinoxes refers to the precession of Earth's axis of rotation with respect to inertial space.
Hipparchus discovered that the positions of the equinoxes move westward along the ecliptic compared to the fixed stars on the celestial sphere. The exact dates of his life are not known, but astronomical observations attributed to him date from 147 BC to 127 BC and were described in his writings.
Currently, this annual motion is about 50.3 seconds of arc per year or 1 degree every 71.6 years. The process is slow, but cumulative. A complete precession cycle covers a period of approximately 25,765 years, the so called great Platonic year, during which time the equinox regresses a full 360°. Precessional movement is also the determining factor in the length of an Astrological Age.
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[edit] Changing pole stars
A consequence of the precession is a changing pole star. Currently Polaris is extremely well-suited to mark the position of the north celestial pole, as Polaris is a moderately bright star with a visual magnitude of 2.1 (variable), and it is located within a half degree of the pole.
On the other hand, Thuban in the constellation Draco, which was the pole star in 3000 BC is much less conspicuous at magnitude 3.67 (one-fifth as bright as Polaris); today it is all but invisible in light-polluted urban skies.
The brilliant Vega in the constellation Lyra is often touted as the best north star (when it fulfilled that role around 12000 BC and will do so again around the year AD 14000), however, it never comes closer than 5° to the pole.
When Polaris becomes the north star again around 27800 AD, due to its proper motion it then will be farther away from the pole than it is now, while in 23600 BC it came closer to the pole.
It is more difficult to find the south celestial pole in the sky at this moment, as that area is a particularly bland portion of the sky, and the nominal south pole star is Sigma Octantis, which with magnitude 5.5 is barely visible to the naked eye even under ideal conditions. That will change from the eightieth to the ninetieth centuries, however, when the south celestial pole travels through the False Cross.
This situation also is seen on a star map, the south pole, which nicely has been pointed to by the Southern cross for the last 2,000 years or so, is moving toward that constellation. By consequence, it is now no longer visible from subtropical northern latitudes, as it was in the time of the ancient Greeks.
[edit] Polar shift and equinoxes shift
The figures to the right attempt to explain the relation between the precession of the Earth's axis and the shift in the equinoxes. These figures show the position of the Earth's axis on the celestial sphere, a fictitious sphere which places the stars according to their position as seen from Earth, regardless of their actual distance. The first image shows the celestial sphere from the outside, with the constellations in mirror image. The second figure shows the perspective of a near-Earth position as seen through a very wide angle lens (from which the apparent distortion).
The rotation axis of the Earth describes, over a period of 25,700 years, a small circle (blue) among the stars, centered around 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. The direction of precession is opposite to the daily rotation of the Earth on its axis. The orange axis was the Earth's rotation axis 5,000 years ago, when it pointed to the star Thuban. The yellow axis, pointing to Polaris, marks the axis now.
The equinoxes occur where the celestial equator intersects the ecliptic (red line), that is, where the Earth's axis is perpendicular to the line connecting the centers of the Sun and Earth. When the axis precesses from one orientation to another, the equatorial plane of the Earth (indicated by the circular grid around the equator) moves. The celestial equator is just the Earth's equator projected onto the celestial sphere, so it moves as the Earth's equatorial plane moves, and the intersection with the ecliptic moves with it. The positions of the poles and equator on Earth do not change, only the orientation of the Earth against the fixed stars.
As seen from the orange grid, 5,000 years ago, the vernal equinox was close to the star Aldebaran of Taurus. Now, as seen from the yellow grid, it has shifted (indicated by the red arrow) to somewhere in the constellation of Pisces.
Still pictures like these are only first approximations as they do not take into account the variable speed of the precession, the variable obliquity of the ecliptic, the planetary precession (whose center lies on a circle about 6° away from the poles) and the proper motions of the stars.
[edit] Explanation
The precession of the equinoxes is caused by the differential gravitational forces of the Sun and the Moon on the Earth.
In popular science books, precession is often explained with the example of a spinning top. While the physical effect is the same, some crucial details differ. For a spinning top, gravity causes the top to wobble, which in turn causes precession. The applied force in this case is parallel to the rotation axis. For the Earth, however, the applied forces of the Sun and the Moon are perpendicular to the axis of rotation.
The Sun and the Moon pull on the equatorial bulge; due to its own rotation, the Earth is not a perfect sphere but an oblate spheroid, with an equatorial diameter about 43 kilometers larger than its polar diameter. If the Earth were a perfect sphere, there would be no precession.
The figure below explains how this process works. (Viewing the diagram at its maximum resolution is recommended.) The Earth is given as a perfect sphere with the mass of the bulge approximated by a blue torus around its equator. The green arrows indicate the gravitational forces from the Sun on some extreme points. These forces are not parallel, as they all point toward the center of the Sun. Therefore, the forces working on the northernmost and southernmost parts of the equatorial bulge have a component perpendicular to the ecliptical plane and a component directed parallel to it. The parallel component is centripetal force for the Earth in its orbit around the Sun. The perpendicular components are shown as cyan arrows tangential to the Earth's surface. These tangential forces create a torque (orange), and this torque, added to the rotation (magenta), shifts the rotational axis to a slightly new position (yellow). Over time, the axis precesses along the white circle, which is centered around the ecliptic pole.
This torque is always in the same direction, perpendicular to the direction in which the rotation axis is tilted away from the ecliptic pole, so that it does not change the axial tilt itself. The magnitude of the torque from the sun (or the moon) varies with the gravitational object's alignment with the earth's spin axis and approaches zero when it is orthogonal.
Although the above explanation involved the Sun, the same explanation holds true for any object moving around the Earth, along or close to the ecliptic, notably, the Moon. The combined action of the Sun and the Moon is called the lunisolar precession. In addition to the steady progressive motion (resulting in a full circle in 25,700 years) the Sun and Moon also cause small periodic variations, due to their changing positions. These oscillations, in both precessional speed and axial tilt, are known as the nutation. The most important term has a period of 18.6 years and an amplitude of less than 20 seconds of arc.
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. This planetary precession shift is only 0.47 seconds of arc per year (more than a hundred times smaller than lunisolar precession), and takes place along the instantaneous equator.
The sum of the two precessions is known as the general precession.
[edit] Climatic effects
The figure to the right illustrates the effects of axial precession on the northern hemisphere seasons, relative to perihelion and aphelion. The precession of the equinoxes contributes to periodic climate change, and is known as the Milankovitch cycle.
Notice in the above figure that the areas swept during a specific season changes through time. Orbital mechanics require that the length of the seasons be proportional to the swept areas of the seasonal quadrants, so when the orbital eccentricity is extreme, the seasons on the far side of the orbit may be substantially longer in duration. Today, in the northern hemisphere, when fall and winter occur at closest approach, the earth is moving at its maximum velocity and therefore, fall and winter are slightly shorter than spring and summer. Today, the northern hemisphere summer is 4.66 days longer than its associated winter and spring is 2.9 days longer than fall.(source) Axial precession slowly changes the place in the Earth's orbit where the solstices and equinoxes occur. See tropical year for a more extensive treatment and numerical values. Over the next 10,000 years, northern hemisphere winters will become gradually longer and northern hemisphere summers will become shorter, eventually creating conditions believed to be favorable for triggering the next ice age.
[edit] History
Precession causes the cycle of seasons (tropical year) to be about 20.4 minutes less than the time for the Earth to return to the same position with respect to the stars. This results in a slow change (one day every 71 calendar years) in the position of the Sun with respect to the stars at an equinox.
Hipparchus estimated the Earth's precession around 130 BC, adding his own observations to those of Babylonian astronomers in the preceding centuries. In particular, they measured the distance of stars such as Spica to the Moon and the Sun during lunar eclipses, and because he could compute the distance of the Moon and the Sun from the equinox at these moments, he noticed that Spica and other stars appeared to have moved over the centuries.
It remains controversial as to whether the ancient Egyptians knew of the Precession or not. Michael Rice wrote in his Egypt's Legacy, "Whether or not the ancients knew of the mechanics of the Precession before its definition by Hipparchos the Bithynian in the second century BC is uncertain, but as dedicated watchers of the night sky they could not fail to be aware of its effects." (p. 128) Rice believes that "the Precession is fundamental to an understanding of what powered the development of Egypt" (p. 10), to the extent that "in a sense Egypt as a nation-state and the king of Egypt as a living god are the products of the realisation by the Egyptians of the astronomical changes effected by the immense apparent movement of the heavenly bodies which the Precession implies." (p. 56) Following Carl Gustav Jung, Rice says that "the evidence that the most refined astronomical observation was practised in Egypt in the third millennium BC (and probably even before that date) is clear from the precision with which the Pyramids at Giza are aligned to the cardinal points, a precision which could only have been achieved by their alignment with the stars. This fact alone makes Jung's belief in the Egyptians' knowledge of the Precession a good deal less speculative than once it seemed." (p. 31) The Egyptians also, says Rice, were "to alter the orientation of a temple when the star on whose position it had originally been set moved its position as a consequence of the Precession, something which seems to have happened several times during the New Kingdom." (p. 170) see also Royal Arch and the Precession of the Equinoxes
[edit] Values
Simon Newcomb's calculation at the end of the nineteenth century for general precession (known as p) in longitude gave a value of 5,025.64 arcseconds per tropical century, and was the generally accepted value until artificial satellites delivered more accurate observations and electronic computers allowed more elaborate models to be calculated. Lieske developed an updated theory in 1976, where p equals 5,029.0966 arcseconds per Julian century. Modern techniques such as VLBI and LLR allowed further refinements, and the International Astronomical Union adopted a new constant value in 2000, and new computation methods and polynomial expressions in 2003 and 2006; the accumulated precession is:
pA = 5,028.796195×T + 1.1054348×T2 + higher order terms,
in arcseconds per Julian century, with T, the time in Julian centuries (that is, 36,525 days) since the epoch of 2000.
The rate of precession is the derivative of that:
p = 5,028.796195 + 2.2108696×T + higher order terms
The constant term of this speed corresponds to one full precession circle in 25,772 years.
The precession rate is not a constant, but slowly increasing over time because of the linear (and higher order) terms in T. In any case it must be stressed that this formula is valid, only over a limited time period. It is clear that if T gets large enough (far in the future or far in the past), the T² term will dominate and p will go to very large values. In reality, more elaborate calculations on the numerical model of solar system show that the precessional constants have a period of about 41,000 years, the same as the obliquity of the ecliptic. Note that the constants mentioned here are the linear and all higher terms of the formula above, not the precession itself. That is, p = A + BT + CT² + … is an approximation of p = A + Bsin (2πT/P), where P is the 410-century period.
Theoretical models may calculate values for p that have high powers of T, but since no (finite) polynomial may ever represent a periodic function, they all go to either positive or negative infinity for large enough T. In that respect, the International Astronomical Union chose the best developed available theory. For up to a few centuries in the past and the future, all formulas do not diverge very much. For up to a few thousand years in the past and the future, most agree to some accuracy. For eras farther out, discrepancies become too large - the exact rate and period of precession may not be computed, even for a single whole precession period.
The precession of Earth's axis is a very slow effect, but at the level of accuracy at which astronomers work, it does need to be taken into account on a daily basis. Note that although the precession and the tilt of Earth's axis (the obliquity of the ecliptic) are calculated from the same theory and thus, are related to each other, the two movements act independently of each other, moving in mutually perpendicular directions.
Over longer time periods, that is, millions of years, it appears that precession is quasiperiodic at around 25,700 years, however, it will not remain so. According to Ward, when the distance of the Moon, which is continuously increasing from tidal effects, will have gone from the current 60.3 to approximately 66.5 Earth radii in about 1,500 million years, resonances from planetary effects will push precession to 49,000 years at first, and then, when the Moon reaches 68 Earth radii in about 2,000 million years, to 69,000 years. This will be associated with wild swings in the obliquity of the ecliptic as well. Ward, however, used the abnormally large modern value for tidal dissipation. Using the 620-million year average provided by tidal rhythmites of about half the modern value, these resonances will not be reached until about 3,000 and 4,000 million years, respectively. Long before that time (about 2,100 million years from now), due to the increasing luminosity of the Sun, however, the oceans of the Earth will have boiled away, which will alter tidal effects significantly.
[edit] References
- Explanatory supplement to the Astronomical ephemeris and the American ephemeris and nautical almanac
- Precession and the Obliquity of the Ecliptic has a comparison of values predicted by different theories
- A.L. Berger (1976), "Obliquity & precession for the last 5 million years", Astronomy & astrophysics 51, 127
- J.H.Lieske e.a. (1977), "Expressions for the Precession Quantities Based upon the IAU (1976) System of Astronomical Constants. Astronomy & Astrophysics 58, 1..16
- W.R. Ward (1982), "Comments on the long-term stability of the earth's obliquity", Icarus 50, 444
- J.L.Hilton e.a (2006), "Report of the International Astronomical Union Division I Working Group on Precession and the Ecliptic". Celestial Mechanics and Dynamical Astronomy (2006) 94: 351..367
- Rice, Michael (1997), Egypt's Legacy: The archetypes of Western civilization, 3000-30 BC, London and New York.
