Dictionary:
par·al·lax (păr'ə-lăks')  |
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| parallax |
The apparent position of a star among more distant stars changes when viewed from opposite sides of the earth's orbit. (Precision Graphics) |
An apparent change in the direction of an object, caused by a change in observational position that provides a new line of sight.
[French parallaxe, from Greek parallaxis, from parallassein, to change : para-, among; see para-1 + allassein, to exchange (from allos, other).]
parallactic par'al·lac'tic (-lăk'tĭk) adj.| 5min Related Video: parallax |
| Sci-Tech Encyclopedia: Parallax |
The apparent angular displacement of a celestial object due to a change in the position of the observer. With a baseline of known length between two observations, the distance to the object can be determined directly.
The rotation of the Earth or the linear separation of two points on its surface can be used to establish distances within the solar system. The parallax determined is scaled to the equatorial radius of the Earth, which is equal to 6378 km (3963 mi). At the mean distance of the Moon, this baseline subtends an angle of 57′02.61′′, and at the mean distance to the Sun it amounts to 8.794148′′. This latter distance is defined as the astronomical unit and serves as a measure of distances within the solar system. One astronomical unit is 149,597,870.66 ± 0.02 km (92,955,807.25 ± 0.01 mi) in length, and its high precision results from tracking interplanetary space probes. See also Astronomical unit; Earth rotation and orbital motion.
The astronomical unit is the baseline for the measure of stellar parallaxes or distances and ultimately every other distance in the universe outside the solar system. Observations made from the Earth in its orbit on opposite sides of the Sun are scaled to the astronomical unit. The stellar parallax is given in units of arc-seconds and is by definition the reciprocal of the distance in parsecs. One parsec is the distance at which one astronomical unit subtends an angle of one second of arc and equals 206,264.8 astronomical units or 3.2616 light-years. See also Light-year; Parsec.
In 1989 the European Space Agency launched the first space satellite entirely devoted to astrometry, named HIPPARCOS (from High Precision Parallax Collecting Satellite, and also honoring the ancient astronomer Hipparchus). In 1993 it completed its mission by obtaining positions, parallaxes, and proper motions for 118,322 stars listed in its final catalog. Its precision averages about ±0.0015′′ for stars brighter than its completeness limit of about the 8th magnitude, and rises to perhaps twice that amount at its ultimate limiting magnitude of 12. This precision is about equal to that of the best of current ground-based work for the brighter stars and less for faint stars. The advantage of HIPPARCOS lies in the much greater numbers of stars, including all the bright ones, with quality parallaxes. The contributions to stellar knowledge from this satellite are enormous. See also Binary star; Hertzsprung-Russell diagram; Satellite (astronomy).
Distance estimates are possible based on the assumption that the apparent mean space motion of a large number of stars with similar characteristics is a reflection of the peculiar motion of the Sun, derived from previous observations. Two related methods apply; the first equates the mean drift of the stars to the Sun's motion vector. The second requires measurements of radial velocities as well as proper motions, and assumes that the radial velocity distribution at the solar apex and antapex (the directions toward and away from which the Sun is moving, respectively) matches that in the transverse velocities along the direction normal to that of the assumed solar motion. These methods are referred to as secular and statistical parallax, respectively, although the terms are sometimes confused.
Several methods for the establishment of distance are frequently and incorrectly labeled parallax. These methods, such as spectroscopic or photometric parallax, involve a comparison of an object to another of known distance and like luminosity, and scaling the distance as necessary. See also Astrometry.
| Dental Dictionary: parallax |
The apparent change in position of an object when viewed from two different positions. The phenomenon is useful in determining the relative position of an object in a radiograph. Two or more radiographs are made from slightly different positions and the direction and amount of shift of the object is observed and measured.
| Britannica Concise Encyclopedia: parallax |
For more information on parallax, visit Britannica.com.
| Archaeology Dictionary: parallax |
The apparent movement of an object when seen from different positions. The effect of parallax can easily be seen by looking at a nearby object with first the left and then the right eye. Taking account of parallax is important in archaeology when planning features on site, drawing objects, and making observations relating to alignment and intervisibility.
| Sports Science and Medicine: parallax |
An optical effect that contributes to the perception of relative distances. Parallax occurs when movement at right angles to the line of vision alters the relative position of two unequally distant objects. The same effect is achieved by the difference in view point of the two eyes when the distance between the eyes relative to the distance of the objects is significant.
| Columbia Encyclopedia: parallax |
| Cosmic Lexicon: Parallax |
Apparent motion of a nearby object as projected against more distant background objects due to the motion of the observer.
| Wikipedia: Parallax |
Parallax is an apparent displacement or difference of orientation of an object viewed along two different lines of sight, and is measured by the angle or semi-angle of inclination between those two lines.[1][2] The term is derived from the Greek παράλλαξις (parallaxis), meaning "alteration". Nearby objects have a larger parallax than more distant objects when observed from different positions, so parallax can be used to determine distances. In astronomy, parallax is the only direct method by which distances to objects (typically stars) beyond the Solar System can be measured. The Hipparcos satellite has used the technique for over 100,000 nearby stars. This provides the basis for all other distance measurements in astronomy, the cosmic distance ladder. Here, the term "parallax" is the angle or semi-angle of inclination between two sightlines to the star.
Parallax also affects optical instruments such as binoculars, microscopes, and twin-lens reflex cameras that view objects from slightly different angles. Many animals, including humans, have two eyes with overlapping visual fields to use parallax to gain depth perception; this process is known as stereopsis.
A simple everyday example of parallax can be seen in the dashboard of motor vehicles that use a "needle" type speedometer gauge (when the needle is mounted in front of its dial scale in a way that leaves a noticeable spacing between them). When viewed from directly in front, the speed may show 60 (i.e. the needle appears against the '60' mark on the dial behind); but when viewed from the passenger seat (i.e. from an oblique angle) the needle can appear against a slightly lower or higher mark (depending on whether it is viewed from the left or from the right), because of the combined effect of the spacing and the angle of view.
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On an interstellar scale, parallax created by the different orbital positions of the Earth causes nearby stars to appear to move relative to more distant stars. By observing parallax, measuring angles and using geometry, one can determine the distance to various objects. When the object in question is a star, the effect is known as stellar parallax.
Stellar parallax is most often measured using annual parallax, defined as the difference in position of a star as seen from the Earth and Sun, i. e. the angle subtended at a star by the mean radius of the Earth's orbit around the Sun. The parsec (3.26 light-years) is defined as the distance for which the annual parallax is 1 arcsecond. Annual parallax is normally measured by observing the position of a star at different times of the year as the Earth moves through its orbit. Measurement of annual parallax was the first reliable way to determine the distances to the closest stars. The first successful measurements of stellar parallax were made by Friedrich Bessel in 1838 for the star 61 Cygni using a heliometer.[3] Stellar parallax remains the standard for calibrating other measurement methods. Accurate calculations of distance based on stellar parallax require a measurement of the distance from the Earth to the Sun, now based on radar reflection off the surfaces of planets.[4]
The angles involved in these calculations are very small and thus difficult to measure. The nearest star to the Sun (and thus the star with the largest parallax), Proxima Centauri, has a parallax of 0.77233 ± 0.00242 arcsec.[5][6] This angle is approximately that subtended by an object 2 centimeters in diameter located 5.3 kilometers away.
The fact that stellar parallax was so small that it was unobservable at the time was used as the main scientific argument against heliocentrism during the early modern age. It is clear from Euclid's geometry that the effect would be undetectable if the stars were far enough away, but for various reasons such gigantic distances involved seemed entirely implausible: it was one of Tycho's principal objections to Copernican heliocentrism that in order for it to be compatible with the lack of observable stellar parallax, there would have to be an enormous and unlikely void between the orbit of Saturn and the eighth sphere (the fixed stars).[7]
In 1989, the satellite Hipparcos was launched primarily for obtaining parallaxes and proper motions of nearby stars, increasing the reach of the method tenfold. Even so, Hipparcos is only able to measure parallax angles for stars up to about 1,600 light-years away, a little more than one percent of the diameter of our galaxy. The European Space Agency's Gaia mission, due to launch in 2011 and come online in 2012, will be able to measure parallax angles to an accuracy of 10 microarcseconds, thus mapping nearby stars (and potentially planets) up to a distance of tens of thousands of light-years from earth.[8]
Distance measurement by parallax is a special case of the principle of triangulation, which states that one can solve for all the sides and angles in a network of triangles if, in addition to all the angles in the network, the length of at least one side has been measured. Thus, the careful measurement of the length of one baseline can fix the scale of an entire triangulation network. In parallax, the triangle is extremely long and narrow, and by measuring both its shortest side (the motion of the observer) and the small top angle (always less than 1 arcsecond,[3] leaving the other two close to 90 degrees), the length of the long sides (in practice considered to be equal) can be determined.
Assuming the angle is small (see derivation below), the distance to an object (measured in parsecs) is the reciprocal of the parallax (measured in arcseconds): d(pc) = 1 / p(arcsec). For example, the distance to Proxima Centauri is 1/0.772=1.29 parsecs (4.2 ly).
Lunar parallax (often short for lunar horizontal parallax or lunar equatorial horizontal parallax), is a special case of parallax: the Moon seen from different viewing positions on the Earth (at one given moment) can appear differently placed against the background of fixed stars.
The diagram (above) for stellar parallax can illustrate lunar parallax as well, if the diagram is taken to be scaled right down and slightly modified. Instead of 'near star', read 'Moon', and instead of taking the circle at the bottom of the diagram to represent the size of the Earth's orbit around the Sun, take it to be the size of the Earth's globe, and of a circle around the Earth's surface. Then, the lunar (horizontal) parallax amounts to the difference in angular position, relative to the background of distant stars, of the Moon as seen from two different viewing positions on the Earth:- one of the viewing positions is the place from which the Moon can be seen directly overhead at a given moment (that is, viewed along the vertical line in the diagram); and the other viewing position is a place from which the Moon can be seen on the horizon at the same moment (that is, viewed along one of the diagonal lines, from an Earth-surface position corresponding roughly to one of the blue dots on the modified diagram).
The lunar (horizontal) parallax can alternatively be defined as the angle subtended at the distance of the Moon by the radius of the Earth[9] -- equal to angle p in the diagram when scaled-down and modified as mentioned above.
The lunar horizontal parallax at any time depends on the linear distance of the Moon from the Earth. The Earth-Moon linear distance varies continuously as the Moon follows its perturbed and approximately elliptical orbit around the Earth. The range of the variation in linear distance is from about 56 to 63.7 earth-radii, corresponding to horizontal parallax of about a degree of arc, but ranging from about 61.4' to about 54'.[10] The Astronomical Almanac and similar publications tabulate the lunar horizontal parallax and/or the linear distance of the Moon from the Earth on a periodical e.g. daily basis for the convenience of astronomers (and formerly, of navigators), and the study of the way in which this coordinate varies with time forms part of lunar theory.
Parallax can also be used to determine the distance to the Moon.
One way to determine the lunar parallax from one location is by using a lunar eclipse. A full shadow of the Earth on the Moon has an apparent radius of curvature equal to the difference between the apparent radii of the Earth and the Sun as seen from the Moon. This radius can be seen to be equal to 0.75 degree, from which (with the solar apparent radius 0.25 degree) we get an Earth apparent radius of 1 degree. This yields for the Earth-Moon distance 60 Earth radii or 384,000 km. This procedure was first used by Aristarchus of Samos[11] and Hipparchus, and later found its way into the work of Ptolemy.[citation needed] The diagram at right shows how daily lunar parallax arises on the geocentric and geostatic planetary model in which the Earth is at the centre of the planetary system and does not rotate. It also illustrates the important point that parallax need not be caused by any motion of the observer, contrary to some definitions of parallax that say it is, but may arise purely from motion of the observed.
Another method is to take two pictures of the Moon at exactly the same time from two locations on Earth and compare the positions of the Moon relative to the stars. Using the orientation of the Earth, those two position measurements, and the distance between the two locations on the Earth, the distance to the Moon can be triangulated:
This is the method referred to by Jules Verne in From the Earth to the Moon:
Up till then, many people had no idea how one could calculate the distance separating the Moon from the Earth. The circumstance was exploited to teach them that this distance was obtained by measuring the parallax of the Moon. If the word parallax appeared to amaze them, they were told that it was the angle subtended by two straight lines running from both ends of the Earth's radius to the Moon. If they had doubts on the perfection of this method, they were immediately shown that not only did this mean distance amount to a whole two hundred thirty-four thousand three hundred and forty-seven miles (94,330 leagues), but also that the astronomers were not in error by more than seventy miles (≈ 30 leagues).
After Copernicus proposed his heliocentric system, with the Earth in revolution around the Sun, it was possible to build a model of the whole solar system without scale. To ascertain the scale, it is necessary only to measure one distance within the solar system, e.g., the mean distance from the Earth to the Sun (now called an astronomical unit, or AU). When found by triangulation, this is referred to as the solar parallax, the difference in position of the Sun as seen from the Earth's centre and a point one Earth radius away, i. e., the angle subtended at the Sun by the Earth's mean radius. Knowing the solar parallax and the mean Earth radius allows one to calculate the AU, the first, small step on the long road of establishing the size and expansion age[12] of the visible Universe.
A primitive way to determine the distance to the Sun in terms of the distance to the Moon was already proposed by Aristarchus of Samos in his book On the Sizes and Distances of the Sun and Moon. He noted that the Sun, Moon, and Earth form a right triangle (right angle at the Moon) at the moment of first or last quarter moon. He then estimated that the Moon, Earth, Sun angle was 87°. Using correct geometry but inaccurate observational data, Aristarchus concluded that the Sun was slightly less than 20 times farther away than the Moon. The true value of this angle is close to 89° 50', and the Sun is actually about 390 times farther away.[11] He pointed out that the Moon and Sun have nearly equal apparent angular sizes and therefore their diameters must be in proportion to their distances from Earth. He thus concluded that the Sun was around 20 times larger than the Moon; this conclusion, although incorrect, follows logically from his incorrect data. It does suggest that the Sun is clearly larger than the Earth, which could be taken to support the heliocentric model. Although these results were incorrect due to observational errors, they were based on correct geometric principles of parallax, and became the basis for estimates of the size of the solar system for almost 2000 years, until the transit of Venus was correctly observed in 1761 and 1769.[11]
This method was proposed by Edmond Halley in 1716, although he did not live to see the results.
The use of Venus transits was less successful than had been hoped due to the black drop effect, but the resulting estimate, 153 million kilometers, is just 2% above the currently accepted value, 149.6 million kilometers.
Much later, the Solar System was 'scaled' using the parallax of asteroids, some of which, like Eros, pass much closer to Earth than Venus. In a favourable opposition, Eros can approach the Earth to within 22 million kilometres.[13] Both the opposition of 1901 and that of 1930/1931 were used for this purpose, the calculations of the latter determination being completed by Astronomer Royal Sir Harold Spencer Jones.[14]
Also radar reflections, both off Venus (1958) and off asteroids, like Icarus, have been used for solar parallax determination. Today, use of spacecraft telemetry links has solved this old problem. The currently accepted value of solar parallax is 8".794 143.[15]
The open stellar cluster Hyades in Taurus extends over such a large part of the sky, 20 degrees, that the proper motions as derived from astrometry appear to converge with some precision to a perspective point north of Orion. Combining the observed apparent (angular) proper motion in seconds of arc with the also observed true (absolute) receding motion as witnessed by the Doppler redshift of the stellar spectral lines, allows estimation of the distance to the cluster (151 light-years) and its member stars in much the same way as using annual parallax.[16]
Dynamic parallax has sometimes also been used to determine the distance to a supernova, when the optical wave front of the outburst is seen to propagate through the surrounding dust clouds at an apparent angular velocity, while its true propagation velocity is known to be the speed of light.[17]
For a right triangle,
where p is the parallax, 1 AU (149,600,000 km) is approximately the average distance from the Sun to Earth, and d is the distance to the star. Using small-angle approximations (valid when the angle is small compared to 1 radian),
so the parallax, measured in arcseconds, is
If the parallax is 1", then the distance is
This defines the parsec, a convenient unit for measuring distance using parallax. Therefore, the distance, measured in parsecs, is simply d = 1 / p, when the parallax is given in arcseconds.[18]
Precise parallax measurements of distance have an associated error. However this error in the measured parallax angle does not translate directly into an error for the distance, except for relatively small errors. The reason for this is that an error toward a smaller angle results in a greater error in distance than an error toward a larger angle.
However, an approximation of the distance error can be computed by
where d is the distance and p is the parallax. The approximation is far more accurate for parallax errors that are small relative to the parallax than for relatively large errors.
Because the eyes of humans and other highly evolved animals are in different positions on the head, they present different views simultaneously. This is the basis of stereopsis, the process by which the brain exploits the parallax due to the different views from the eye to gain depth perception and estimate distances to objects.[19] Animals also use motion parallax, in which the animal (or just the head) moves to gain different viewpoints. For example, pigeons (whose eyes do not have overlapping fields of view and thus cannot use stereopsis) bob their heads up and down to see depth.[20]
If an optical instrument — e.g., a telescope, microscope, or theodolite — is imprecisely focused, its cross-hairs will appear to move with respect to the object focused on if one moves one's head horizontally in front of the eyepiece. This is why it is important, especially when performing measurements, to focus carefully in order to eliminate the parallax, and to check by moving one's head.
Also, in non-optical measurements the thickness of a ruler can create parallax in fine measurements. To avoid parallax error, one should take measurements with one's eye on a line directly perpendicular to the ruler so that the thickness of the ruler does not create error in positioning for fine measurements. A similar error can occur when reading the position of a pointer against a scale in an instrument such as a galvanometer. To help the user avoid this problem, the scale is sometimes printed above a narrow strip of mirror, and the user positions his eye so that the pointer obscures its own reflection. This guarantees that the user's line of sight is perpendicular to the mirror and therefore to the scale.
Parallax can cause a speedometer reading to appear different to a car's passenger than to the driver.
Aerial picture pairs, when viewed through a stereo viewer, offer a pronounced stereo effect of landscape and buildings. High buildings appear to 'keel over' in the direction away from the centre of the photograph. Measurements of this parallax are used to deduce the height of the buildings, provided that flying height and baseline distances are known. This is a key component to the process of photogrammetry.
Parallax error can be seen when taking photos with many types of cameras, such as twin-lens reflex cameras and those including viewfinders (such as rangefinder cameras). In such cameras, the eye sees the subject through different optics (the viewfinder, or a second lens) than the one through which the photo is taken. As the viewfinder is often found above the lens of the camera, photos with parallax error are often slightly lower than intended, the classic example being the image of person with his or her head cropped off. This problem is addressed in single-lens reflex cameras, in which the viewfinder sees through the same lens through which the photo is taken (with the aid of a movable mirror), thus avoiding parallax error.
In many early graphical applications, such as video games, the scene was constructed of independent layers that were scrolled at different speeds when the player/cursor moved. Some hardware had explicit support for such layers, such as the Super Nintendo Entertainment System. This gave some layers the appearance of being farther away than others and was useful for creating an illusion of depth, but only worked when the player was moving. Now, most games are based on much more comprehensive three-dimensional graphic models, although portable game systems (DS) still often use parallax.
Owing to the positioning of gun turrets on a warship, each has a slightly different perspective of the target relative to the ship itself. Therefore, the ship's system for aiming its guns must compensate for parallax in order to assure that fire from each turret converges on the target.
In a philosophic/geometric sense: An apparent change in the direction of an object, caused by a change in observational position that provides a new line of sight. The apparent displacement, or difference of position, of an object, as seen from two different stations, or points of view. In contemporary writing parallax can also be the same story, or a similar story from approximately the same time line, from one book told from a different perspective in another book. The word and concept feature prominently in James Joyce's 1922 novel, Ulysses. Orson Scott Card also used the term when referring to Ender's Shadow as compared to Ender's Game.
The metaphor is invoked by Slovenian philosopher Slavoj Žižek in his work The Parallax View. Žižek borrowed the concept of "parallax view" from the Japanese philosopher and literary critic Kojin Karatani. "The philosophical twist to be added (to parallax), of course, is that the observed distance is not simply subjective, since the same object that exists 'out there' is seen from two different stances, or points of view. It is rather that, as Hegel would have put it, subject and object are inherently mediated so that an 'epistemological' shift in the subject's point of view always reflects an ontological shift in the object itself. Or—to put it in Lacanese—the subject's gaze is always-already inscribed into the perceived object itself, in the guise of its 'blind spot,' that which is 'in the object more than object itself', the point from which the object itself returns the gaze. Sure the picture is in my eye, but I am also in the picture."[21]
The word is used in the title of Alan J. Pakula's 1974 movie The Parallax View, in which a reporter (Warren Beatty) investigates an assassination. The word in this case refers to a fictional corporation portrayed in the film.
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| Translations: Parallax |
Dansk (Danish)
n. - parallakse
Français (French)
n. - parallaxe
Deutsch (German)
n. - Parallaxe
Ελληνική (Greek)
n. - (αστρον.) παραλλαγή, παράλλαξη
Português (Portuguese)
n. - paralaxe (f)
Español (Spanish)
n. - paralaje
Svenska (Swedish)
n. - parallax
中文（简体）(Chinese (Simplified))
视差
中文（繁體）(Chinese (Traditional))
n. - 視差
한국어 (Korean)
n. - 시차, 패럴렉스 (파인더와 렌즈의 시차)
日本語 (Japanese)
n. - 視差, パララックス
العربيه (Arabic)
(الاسم) إختلاف المنظر, تغير ظاهري في موقع الشيء وبخاصه الجرم السماوي, المنظور, تباحز
עברית (Hebrew)
n. - ההבדל במיקום ובכיוון של עצם כאשר מסתכלים בו מעמדות שונות, עתק (תזוזה)
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