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An apsis (Greek: ἁψίς; plural apsides //, Greek: ἁψῖδες) is an extreme point in the orbit of an object. The word comes via Latin from Greek and is cognate with apse. For elliptic orbits about a larger body, there are two apsides, named with the prefixes peri- (from περί (peri), meaning 'near') and ap-/apo- (from ἀπ(ό) (ap(ó)), meaning 'away from') added to a reference to the body being orbited.
A straight line connecting the periapsis and apoapsis is the line of apsides. This is the major axis of the ellipse, its greatest diameter. The center of mass, or barycenter, of a two-body system lies on this line at one of the two foci of the ellipse. When one body is sufficiently larger than the other, this focus may be located within the larger body. However, whether this is the case, both bodies are in similar elliptical orbits. Both orbits share a common focus at the system's barycenter, with their respective lines of apsides being of length inversely proportional to their masses.
Historically, in geocentric systems, apsides were measured from the center of the Earth. However, in the case of the Moon, the barycenter of the Earth–Moon system (or the Earth–Moon barycenter) as the common focus of both bodies' orbits about each other, is about 75% of the way from Earth's center to its surface.
In orbital mechanics, the apsis technically refers to the distance measured between the barycenters of the central body and orbiting body. However, in the case of spacecraft, the family of terms are commonly used to refer to the orbital altitude of the spacecraft from the surface of the central body (assuming a constant, standard reference radius).
These formulae characterize the pericenter and apocenter of an orbit:
Note that for conversion from heights above the surface to distances between an orbit and its primary, the radius of the central body has to be added, and conversely.
The geometric mean of the two limiting speeds is
which is the speed of a body in a circular orbit whose radius is .
The words "pericenter" and "apocenter" are often seen, although periapsis/apoapsis are preferred in technical usage.
Various related terms are used for other celestial objects. The '-gee', '-helion', '-astron' and '-galacticon' forms are frequently used in the astronomical literature when referring to the Earth, Sun, stars and the Galactic Center respectively. The suffix '-jove' is occasionally used for Jupiter, while '-saturnium' has very rarely been used in the last 50 years for Saturn. The '-gee' form is commonly used as a generic 'closest approach to planet' term instead of specifically applying to the Earth. During the Apollo program, the terms pericynthion and apocynthion (referencing Cynthia, an alternative name for the Greek Moon goddess Artemis) were used when referring to the Moon. Regarding black holes, the term peri/apomelasma (from a Greek root) was used by physicist Geoffrey A. Landis in 1998, before peri/aponigricon (from Latin) appeared in the scientific literature in 2002, as well as peri/apobothron (from Greek bothros, meaning hole or pit).
The following suffixes are added to peri- and apo- to form the terms for the nearest and farthest orbital distances from these objects. For the Solar System objects, only the suffixes for the Earth and Sun are commonly used – the other suffixes are rarely used. Instead, the generic suffix of -apsis is used[not in citation given].
of the name
|Astronomical object||Star||Galaxy||Barycenter||Black hole|
The words perihelion and aphelion were coined by Johannes Kepler to describe the orbital motion of the planets. The words are formed from the prefixes peri- (Greek: περί, near) and apo- (Greek: ἀπό, away from) affixed to the Greek word for the sun, ἥλιος.
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Currently, the Earth reaches perihelion in early January, approximately 14 days after the December Solstice. At perihelion, the Earth's center is about 29 0.983astronomical units (AU) or 147,098,070 km (91,402,500 mi) from the Sun's center. In contrast, the Earth reaches aphelion currently in early July, approximately 14 days after the June Solstice. The aphelion distance between the Earth's and Sun's centers is currently about 71 AU or 152,097,700 km (94,509,100 mi). Dates change over time due to precession and other orbital factors, which follow cyclical patterns known as 1.016Milankovitch cycles. In the short term, the dates of perihelion and aphelion can vary up to 2 days from one year to another. This significant variation is due to the presence of the Moon: while the Earth–Moon barycenter is moving on a stable orbit around the Sun, the position of the Earth's center which is on average about 4,700 kilometres (2,900 mi) from the barycenter, could be shifted in any direction from it – and this affects the timing of the actual closest approach between the Sun's and the Earth's centers (which in turn defines the timing of perihelion in a given year).
Because of the increased distance at aphelion, only 93.55% of the solar radiation from the Sun falls on a given area of land as does at perihelion. However, this fluctuation does not account for the seasons, as it is summer in the northern hemisphere when it is winter in the southern hemisphere and vice versa. Instead, seasons result from the tilt of Earth's axis, which is 23.4 degrees away from perpendicular to the plane of Earth's orbit around the sun. Winter falls on the hemisphere where sunlight strikes least directly, and summer falls where sunlight strikes most directly, regardless of the Earth's distance from the Sun. In the northern hemisphere, summer occurs at the same time as aphelion. Despite this, there are larger land masses in the northern hemisphere, which are easier to heat than the seas. Consequently, summers are 2.3 °C (4 °F) warmer in the northern hemisphere than in the southern hemisphere under similar conditions. Astronomers commonly express the timing of perihelion relative to the vernal equinox not in terms of days and hours, but rather as an angle of orbital displacement, the so-called longitude of the periapsis (also called longitude of the pericenter). For the orbit of the Earth, this is called the longitude of perihelion, and in 2000 it was about 282.895°; by the year 2010, this had advanced by a small fraction of a degree to about 283.067°.
For the orbit of the Earth around the Sun, the time of apsis is often expressed in terms of a time relative to seasons, since this determines the contribution of the elliptical orbit to seasonal variations. The variation of the seasons is primarily controlled by the annual cycle of the elevation angle of the Sun, which is a result of the tilt of the axis of the Earth measured from the plane of the ecliptic. The Earth's eccentricity and other orbital elements are not constant, but vary slowly due to the perturbing effects of the planets and other objects in the solar system. See Milankovitch cycles. On a very long time scale, the dates of the perihelion and of the aphelion progress through the seasons, and they make one complete cycle in 22,000 to 26,000 years. There is a corresponding movement of the position of the stars as seen from Earth that is called the apsidal precession. (This is closely related to the precession of the axis.) The dates and times of the perihelions and aphelions for several past and future years are listed in the following table:
|Date||Time (UT)||Date||Time (UT)|
|2007||January 3||19:43||July 6||23:53|
|2008||January 2||23:51||July 4||07:41|
|2009||January 4||15:30||July 4||01:40|
|2010||January 3||00:09||July 6||11:30|
|2011||January 3||18:32||July 4||14:54|
|2012||January 5||00:32||July 5||03:32|
|2013||January 2||04:38||July 5||14:44|
|2014||January 4||11:59||July 4||00:13|
|2015||January 4||06:36||July 6||19:40|
|2016||January 2||22:49||July 4||16:24|
|2017||January 4||14:18||July 3||20:11|
|2018||January 3||05:35||July 6||16:47|
|2019||January 3||05:20||July 4||22:11|
|2020||January 5||07:48||July 4||11:35|
|Type of body||Body||Distance from Sun at perihelion||Distance from Sun at aphelion|
|Planet||Mercury||46,001,009 km (28,583,702 mi)||69,817,445 km (43,382,549 mi)|
|Venus||107,476,170 km (66,782,600 mi)||108,942,780 km (67,693,910 mi)|
|Earth||147,098,291 km (91,402,640 mi)||152,098,233 km (94,509,460 mi)|
|Mars||206,655,215 km (128,409,597 mi)||249,232,432 km (154,865,853 mi)|
|Jupiter||740,679,835 km (460,237,112 mi)||816,001,807 km (507,040,016 mi)|
|Saturn||1,349,823,615 km (838,741,509 mi)||1,503,509,229 km (934,237,322 mi)|
|Uranus||2,734,998,229 km (1.699449110×109 mi)||3,006,318,143 km (1.868039489×109 mi)|
|Neptune||4,459,753,056 km (2.771162073×109 mi)||4,537,039,826 km (2.819185846×109 mi)|
|Dwarf planet||Ceres||380,951,528 km (236,712,305 mi)||446,428,973 km (277,398,103 mi)|
|Pluto||4,436,756,954 km (2.756872958×109 mi)||7,376,124,302 km (4.583311152×109 mi)|
|Haumea||5,157,623,774 km (3.204798834×109 mi)||7,706,399,149 km (4.788534427×109 mi)|
|Makemake||5,671,928,586 km (3.524373028×109 mi)||7,894,762,625 km (4.905578065×109 mi)|
|Eris||5,765,732,799 km (3.582660263×109 mi)||14,594,512,904 km (9.068609883×109 mi)|
The following chart shows the range of distances of the planets, dwarf planets and Halley's Comet from the Sun.
Distances of selected bodies of the Solar System from the Sun. The left and right edges of each bar correspond to the perihelion and aphelion of the body, respectively, hence long bars denote high orbital eccentricity. The radius of the Sun is 0.7 million km, and the radius of Jupiter (the largest planet) is 0.07 million km, both too small to resolve on this image.
The images below show the perihelion (green dot) and aphelion (red dot) points of the inner and outer planets.
The perihelion and aphelion points of the inner planets of the Solar System
The perihelion and aphelion points of the outer planets of the Solar System
|Look up apsis in Wiktionary, the free dictionary.|