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The apparent place of an object is its position in space as seen by an observer. Because of physical and geometrical effects it may differ from the "true" or "geometric" position.

Astronomy

In astronomy, a distinction is made between the mean position, apparent position and topocentric position of an object.

Position of a star

The mean position of a star (relative to the observer's adopted coordinate system) can be calculated from its value at an arbitrary epoch, together with its actual motion over time (known as proper motion). The apparent position is its position as seen by a theoretical observer at the centre of the moving Earth. Several effects cause the apparent position to differ from the mean position:^[1]

Annual aberration – a deflection caused by the velocity of the Earth's motion around the Sun, relative to an inertial frame of reference. This is independent of the distance of the star from the Earth.
Annual parallax – the apparent change in position due to the star being viewed from different places as the Earth orbits the Sun in the course of a year. Unlike aberration, this effect depends on the distance of the star, being larger for nearby stars.
Precession – a long-term (ca. 26,000 years) variation in the direction of the Earth's axis of rotation.
Nutation – shorter-term variations in the direction of the Earth's axis of rotation.

The Apparent Places of Fundamental Stars is an astronomical yearbook, which is published one year in advance by the Astronomical Calculation Institute (Heidelberg University) in Heidelberg, Germany. It lists the apparent place of about 1000 fundamental stars for every 10 days and is published as a book and in a more extensive version on the Internet.

Solar System objects

The apparent position of a planet or other object in the Solar System is also affected by light-time correction, which is caused by the finite time it takes light from a moving body to reach the observer. Simply put, the observer sees the object in the position where it was when the light left it.

Theoretically, light-time correction could also be calculated for more distant objects, such as stars, but in practice it is ignored. The movement of an object since the light left it is not needed because the mean position is the mean position of where it appears to be, not of where it once was. Unlike planets, these objects basically appear to move in straight lines, so for normal use no complicated calculation is needed to find their mean position.

Topocentric position

The topocentric position of a body is that seen by an actual observer on the Earth, and differs from the apparent position as a result of the following effects:

Diurnal aberration – a deflection caused by the velocity of the observer's motion around the Earth's centre, due to its rotation.
Diurnal parallax – the apparent change in position due to the object being viewed from different places as the observer's position rotates around the Earth's axis.
Polar motion – small changes in the position of the Earth's axis of rotation relative to its surface.
Atmospheric refraction – a deflection of the light from the object caused by its passage through the Earth's atmosphere.

References

^ Seidelmann, P. Kenneth, ed. (1992). Explanatory Supplement to the Astronomical Almanac: A Revision to the Explanatory Supplement to the Astronomical Ephemeris and the American Ephemeris and Nautical Almanac. Sausalito, Ca.: University Science Books. pp. 99–140.

External links

Apparent Places of Fundamental Stars

[ESAA1992-1] Seidelmann, P. Kenneth, ed. (1992). Explanatory Supplement to the Astronomical Almanac: A Revision to the Explanatory Supplement to the Astronomical Ephemeris and the American Ephemeris and Nautical Almanac. Sausalito, Ca.: University Science Books. pp. 99–140.

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-The '''apparent place''' of an [[object (physics)|object]] is the position in space as seen by the [[observation|observer]]. Because of physical and/or geometrical effects it has a [[deviation]] from the "true position".
+The '''apparent place''' of an [[physical body|object]] is its position in space as seen by an observer. Because of physical and geometrical effects it may differ from the "true" or "geometric" position.
+== Astronomy ==
-In [[Astronomy]] the term "apparent places of [[Star | star]]s" means the visual or photographic position of the star, as seen from the moving [[Earth]]. For instance, its speed of 30 km per second around the [[Sun]] causes an [[annual aberration]] of about 20" (10^-4) because the Earth's poocity is about 0.01 percent of the [[speed of light]].
+In [[astronomy]], a distinction is made between the ''mean position'', ''apparent position'' and ''topocentric position'' of an object.
-Other effects are the [[parallax]] (different angle to the star during the [[year]]), or the [[day|daily]] [[aberration]] because of the [[Earth's rotation]], and the Earth's [[precession]] - a monotonic changing of the direction of the Earth's axis, which causes an analogous slow turning of the [[coordinate system]]s which we use on Earth and in [[space]].
+=== Position of a star ===
-The '''"Apparent Places of Fundamental Stars"''' (commonly abbreviated [[APFS]]) is an astronomical [[yearbook]], which is published one year in advance by the [[Astronomisches Rechen-Institut]] in [[Heidelberg]], Germany. It lists the apparent place of about 1000 [[fundamental star]]s for every 10 days and is published as a book and in a more extensive version on the [[Internet]].
+The mean position of a [[star]] (relative to the observer's adopted [[coordinate system]]) can be calculated from its value at an arbitrary [[epoch (astronomy)|epoch]], together with its actual motion over time (known as [[proper motion]]). The ''apparent position'' is its position as seen by a theoretical observer at the centre of the moving [[Earth]]. Several effects cause the apparent position to differ from the mean position:<ref name=ESAA1992>{{cite book|date=1992|editor1-last=Seidelmann|editor1-first=P. Kenneth|title=Explanatory Supplement to the ''Astronomical Almanac'': A Revision to the Explanatory Supplement to the Astronomical Ephemeris and the American Ephemeris and Nautical Almanac|url=https://archive.org/details/131123ExplanatorySupplementAstronomicalAlmanac|location=Sausalito, Ca.|publisher=University Science Books|pages=[https://archive.org/details/131123ExplanatorySupplementAstronomicalAlmanac/page/n64 99]–140}}</ref>
-== See also ==
+* Annual [[Aberration of light|aberration]] – a deflection caused by the [[velocity]] of the Earth's motion around the [[Sun]], relative to an [[inertial frame of reference]]. This is independent of the distance of the star from the Earth.
-* [[Improper motion]]
+* Annual [[parallax]] – the apparent change in position due to the star being viewed from different places as the Earth orbits the Sun in the course of a [[year]]. Unlike aberration, this effect depends on the distance of the star, being larger for nearby stars.
+* [[Axial precession|Precession]] – a long-term (ca. 26,000 years) variation in the direction of the Earth's axis of rotation.
+* [[Nutation]] – shorter-term variations in the direction of the Earth's axis of rotation.
+The ''Apparent Places of Fundamental Stars'' is an astronomical [[yearbook]], which is published one year in advance by the [[Astronomical Calculation Institute (Heidelberg University)]] in [[Heidelberg]], Germany. It lists the apparent place of about 1000 [[fundamental star]]s for every 10 days and is published as a book and in a more extensive version on the [[Internet]].
+=== Solar System objects ===
+The apparent position of a [[planet]] or other object in the [[Solar System]] is also affected by [[light-time correction]], which is caused by the finite time it takes light from a moving body to reach the observer. Simply put, the observer sees the object in the position where it was when the light left it.
+Theoretically, light-time correction could also be calculated for more distant objects, such as stars, but in practice it is ignored. The movement of an object since the light left it is not needed because the mean position is the mean position of where it appears to be, not of where it once was. Unlike planets, these objects basically appear to move in straight lines, so for normal use no complicated calculation is needed to find their mean position.
+=== Topocentric position ===
+The ''topocentric position'' of a body is that seen by an actual observer on the Earth, and differs from the apparent position as a result of the following effects:
+* Diurnal [[Aberration of light|aberration]] – a deflection caused by the [[velocity]] of the observer's motion around the Earth's centre, due to its [[rotation]].
+* Diurnal [[parallax]] – the apparent change in position due to the object being viewed from different places as the observer's position rotates around the Earth's axis.
+* [[Polar motion]] – small changes in the position of the Earth's [[axis of rotation]] relative to its surface.
+* [[Atmospheric refraction]] – a deflection of the light from the object caused by its passage through the Earth's [[atmosphere of Earth|atmosphere]].
+==See also==
 * [[Astrometry]]
-* [[dUT1]]
+* [[Celestial navigation]]
+* [[Coordinated Universal Time]]
+* [[dUT1]]
 * [[Geodetic astronomy]]
-* [[Local apparent time]]
 * [[Meridian circle]]
-* [[Navigation]]
+* [[Solar time]]
-* [[Passage instrument]]
 * [[Star position]]
 * [[Zenith camera]]
-* [[UTC]]
+==References==
+{{Reflist}}
 ==External links==
 *[http://www.ari.uni-heidelberg.de/publikationen/apf/ Apparent Places of Fundamental Stars]
+{{Portal bar|Astronomy|Stars|Spaceflight|Outer space|Solar System}}
 [[Category:Astrometry]]
 [[Category:Geodesy]]
-[[de:Apparent Places]]