apsis#Earth's perihelion and aphelion

File:Periapsis_apoapsis.pngs: The smaller, satellite body (blue) orbits the primary body (yellow); both are in elliptic orbits around their common center of mass (or barycenter), (red +).
∗Periapsis and apoapsis as distances: the smallest and largest distances between the orbiter and its host body.]]

There are two apsides in any elliptic orbit. The name for each apsis is created from the prefixes ap-, apo- ({{ety||ἀπ(ό), (ap(o)-)|away from}}) for the farthest or peri- ({{ety||περί (peri-)|near}}) for the closest point to the primary body, with a suffix that describes the primary body. The suffix for Earth is -gee, so the apsides' names are apogee and perigee. For the Sun, the suffix is -helion, so the names are aphelion and perihelion.

According to Newton's laws of motion, all periodic orbits are ellipses. The barycenter of the two bodies may lie well within the bigger body—e.g., the Earth–Moon barycenter is about 75% of the way from Earth's center to its surface.{{Cite web |title=Earth-Moon Barycenter - SkyMarvels.com |url=https://www.skymarvels.com/gallery/Vid%20-%20Earth-Moon%20Barycenter.htm |access-date=2024-04-23 |website=www.skymarvels.com}} If, compared to the larger mass, the smaller mass is negligible (e.g., for satellites), then the orbital parameters are independent of the smaller mass.

When used as a suffix—that is, -apsis—the term can refer to the two distances from the primary body to the orbiting body when the latter is located: 1) at the periapsis point, or 2) at the apoapsis point (compare both graphics, second figure). The line of apsides denotes the distance of the line that joins the nearest and farthest points across an orbit; it also refers simply to the extreme range of an object orbiting a host body (see top figure; see third figure).

In orbital mechanics, the apsides technically refer to the distance measured between the barycenter of the 2-body system and the center of mass of the orbiting body. However, in the case of a spacecraft, the terms are commonly used to refer to the orbital altitude of the spacecraft above the surface of the central body (assuming a constant, standard reference radius).

Image:Angular Parameters of Elliptical Orbit.png orbital elements: point G, the nearest point of approach of an orbiting body, is the pericenter (also periapsis) of an orbit; point H, the farthest point of the orbiting body, is the apocenter (also apoapsis) of the orbit; and the red line between them is the line of apsides.]]

The words "pericenter" and "apocenter" are often seen, although periapsis/apoapsis are preferred in technical usage.

• For generic situations where the primary is not specified, the terms pericenter and apocenter are used for naming the extreme points of orbits (see table, top figure); periapsis and apoapsis (or apapsis) are equivalent alternatives, but these terms also frequently refer to distances—that is, the smallest and largest distances between the orbiter and its host body (see second figure).
• For a body orbiting the Sun, the point of least distance is the perihelion ({{IPAc-en|ˌ|p|ɛr|ᵻ|ˈ|h|i:|l|i|ə|n}}), and the point of greatest distance is the aphelion ({{IPAc-en|æ|p|ˈ|h|i:|l|i|ə|n}});Since the Sun, Ἥλιος in Greek, begins with a vowel (H is the long ē vowel in Greek), the final o in "apo" is omitted from the prefix. =The pronunciation "Ap-helion" is given in many dictionaries [https://www.oxforddictionaries.com/definition/english/aphelion] {{Webarchive|url=https://web.archive.org/web/20151222075218/https://www.oxforddictionaries.com/definition/english/aphelion|date=December 22, 2015}}, pronouncing the "p" and "h" in separate syllables. However, the pronunciation {{IPAc-en|ə|ˈ|f|iː|l|i|ə|n}} [http://www.dictionary.com/browse/aphelion] {{Webarchive|url=https://web.archive.org/web/20170729001850/http://www.dictionary.com/browse/aphelion|date=July 29, 2017}} is also common (e.g., McGraw Hill Dictionary of Scientific and Technical Terms, 5th edition, 1994, p. 114), since in late Greek, 'p' from ἀπό followed by the 'h' from ἥλιος becomes phi; thus, the Greek word is αφήλιον. (see, for example, Walker, John, A Key to the Classical Pronunciation of Greek, Latin, and Scripture Proper Names, Townsend Young 1859 [https://play.google.com/store/books/details?id=LuF-9HKGbl4C&rdid=book-LuF-9HKGbl4C&rdot=1] {{Webarchive|url=https://web.archive.org/web/20190921013331/https://play.google.com/store/books/details?id=LuF-9HKGbl4C&rdid=book-LuF-9HKGbl4C&rdot=1|date=September 21, 2019}}, page 26.) Many [https://www.merriam-webster.com/dictionary/aphelion] dictionaries give both pronunciations when discussing orbits around other stars the terms become periastron and apastron.
• When discussing a satellite of Earth, including the Moon, the point of least distance is the perigee ({{IPAc-en|ˈ|p|ɛr|ᵻ|dʒ|i:}}), and of greatest distance, the apogee (from Ancient Greek: Γῆ (Gē), "land" or "earth").{{cite EB1911 |wstitle=Perigee |volume=21 |page=149}}
• For objects in lunar orbit, the point of least distance are called the pericynthion ({{IPAc-en|ˌ|p|ɛr|ɪ|ˈ|s|ɪ|n|θ|i|ə|n}}) and the greatest distance the apocynthion ({{IPAc-en|ˌ|æ|p|ə|ˈ|s|ɪ|n|θ|i|ə|n}}). The terms perilune and apolune, as well as periselene and aposelene are also used.{{cite web|url=https://solarsystem.nasa.gov/basics/glossary|title=Basics of Space Flight|publisher=NASA|access-date=May 30, 2017|archive-date=September 30, 2019|archive-url=https://web.archive.org/web/20190930063643/https://solarsystem.nasa.gov/basics/glossary/|url-status=live}} Since the Moon has no natural satellites this only applies to man-made objects.

The words perihelion and aphelion were coined by Johannes KeplerKlein, Ernest, A Comprehensive Etymological Dictionary of the English Language, Elsevier, Amsterdam, 1965. ([https://archive.org/stream/AComprehensiveEtymologicalDictionaryOfTheEnglishLanguageByErnestKlein/A%20Comprehensive%20Etymological%20Dictionary%20of%20the%20English%20Language%20by%20Ernest%20Klein_djvu.txt Archived version]) to describe the orbital motions of the planets around the Sun.

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, or hēlíos).

Various related terms are used for other celestial objects. The suffixes -gee, -helion, -astron and -galacticon 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, but -saturnium has very rarely been used in the last 50 years for Saturn. The -gee form is also used as a generic closest-approach-to "any planet" term—instead of applying it only to Earth.

During the Apollo program, the terms pericynthion and apocynthion were used when referring to orbiting the Moon; they reference Cynthia, an alternative name for the Greek Moon goddess Artemis.{{cite web | title = Apollo 15 Mission Report | work = Glossary | url = https://history.nasa.gov/alsj/a15/a15mr-f.htm | access-date = October 16, 2009 | archive-date = March 19, 2010 | archive-url = https://web.archive.org/web/20100319081116/http://history.nasa.gov/alsj/a15/a15mr-f.htm | url-status = live }} More recently, during the Artemis program, the terms perilune and apolune have been used.{{cite conference |author=R. Dendy |author2=D. Zeleznikar |author3=M. Zemba | title = NASA Lunar Exploration – Gateway's Power and Propulsion Element Communications Links | conference = 38th International Communications Satellite Systems Conference (ICSSC) | date = September 27, 2021 | location = Arlington, VA | url = https://ntrs.nasa.gov/citations/20210019019 | access-date = July 18, 2022 | archive-date = Mar 29, 2022 | archive-url=https://web.archive.org/web/20220329140256/https://ntrs.nasa.gov/citations/20210019019 | url-status = live }}

Regarding black holes, the term peribothron was first used in a 1976 paper by J. Frank and M. J. Rees,{{cite journal |author1=Frank, J. |author2=Rees, M.J. |title=Effects of massive black holes on dense stellar systems. |journal=MNRAS |volume=176 |pages=633–646 |date=September 1, 1976 |issue=6908 |doi=10.1093/mnras/176.3.633|bibcode=1976MNRAS.176..633F|doi-access=free }} who credit W. R. Stoeger for suggesting creating a term using the greek word for pit: "bothron".

The terms perimelasma and apomelasma (from a Greek root) were used by physicist and science-fiction author Geoffrey A. Landis in a story published in 1998,[http://www.infinityplus.co.uk/stories/perimelasma.htm Perimelasma] {{Webarchive|url=https://web.archive.org/web/20190225210759/http://www.infinityplus.co.uk/stories/perimelasma.htm |date=February 25, 2019 }}, by Geoffrey Landis, first published in Asimov's Science Fiction, January 1998, republished at Infinity Plus thus appearing before perinigricon and aponigricon (from Latin) in the scientific literature in 2002.{{cite journal |author=R. Schödel |author2=T. Ott |author3=R. Genzel |author4=R. Hofmann |author5=M. Lehnert |author6=A. Eckart |author7=N. Mouawad |author8=T. Alexander |author9=M. J. Reid |author10=R. Lenzen |author11=M. Hartung |author12=F. Lacombe |author13=D. Rouan |author14=E. Gendron |author15=G. Rousset |author16=A.-M. Lagrange |author17=W. Brandner |author18=N. Ageorges |author19=C. Lidman |author20=A. F. M. Moorwood |author21=J. Spyromilio |author22=N. Hubin |author23=K. M. Menten |title=A star in a 15.2-year orbit around the supermassive black hole at the centre of the Milky Way |journal=Nature |volume=419 |pages=694–696 |date=October 17, 2002 |issue=6908 |doi=10.1038/nature01121|arxiv=astro-ph/0210426 |bibcode=2002Natur.419..694S |pmid=12384690|s2cid=4302128 }}

The suffixes shown below may be added to prefixes peri- or apo- to form unique names of apsides for the orbiting bodies of the indicated host/(primary) system. However, only for the Earth, Moon and Sun systems are the unique suffixes commonly used. Exoplanet studies commonly use -astron, but typically, for other host systems the generic suffix, -apsis, is used instead.{{cite web |url=http://lasp.colorado.edu/home/maven/science/science-orbit/|title=MAVEN » Science Orbit|access-date=November 7, 2018|archive-date=November 8, 2018|archive-url=https://web.archive.org/web/20181108025706/http://lasp.colorado.edu/home/maven/science/science-orbit/|url-status=live}}{{Failed verification|date=January 2019| reason=Reference is simply one example of the use of -apsis for an orbit around Mars}}

{{Redirect|Perihelion}}

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File:Perihelion-Aphelion.svg around the Sun with its nearest (perihelion) and farthest (aphelion) points]]

The perihelion (q) and aphelion (Q) are the nearest and farthest points respectively of a body's direct orbit around the Sun.

Comparing osculating elements at a specific epoch to those at a different epoch will generate differences. The time-of-perihelion-passage as one of six osculating elements is not an exact prediction (other than for a generic two-body model) of the actual minimum distance to the Sun using the full dynamical model. Precise predictions of perihelion passage require numerical integration.

The two images below show the orbits, orbital nodes, and positions of perihelion (q) and aphelion (Q) for the planets of the Solar System{{cite web|title=the definition of apsis|url=http://dictionary.reference.com/browse/apsis|website=Dictionary.com|access-date=November 28, 2015|archive-date=December 8, 2015|archive-url=https://web.archive.org/web/20151208101127/http://dictionary.reference.com/browse/apsis|url-status=live}} as seen from above the northern pole of Earth's ecliptic plane, which is coplanar with Earth's orbital plane. The planets travel counterclockwise around the Sun and for each planet, the blue part of their orbit travels north of the ecliptic plane, the pink part travels south, and dots mark perihelion (green) and aphelion (orange).

The first image (below-left) features the inner planets, situated outward from the Sun as Mercury, Venus, Earth, and Mars. The reference Earth-orbit is colored yellow and represents the orbital plane of reference. At the time of vernal equinox, the Earth is at the bottom of the figure. The second image (below-right) shows the outer planets, being Jupiter, Saturn, Uranus, and Neptune.

The orbital nodes are the two end points of the "line of nodes" where a planet's tilted orbit intersects the plane of reference;{{cite encyclopedia |url=http://www.daviddarling.info/encyclopedia/L/line_of_nodes.html |title=line of nodes |encyclopedia=The Encyclopedia of Astrobiology, Astronomy, and Spaceflight |first=David |last=Darling |access-date=May 17, 2007 |archive-date=August 23, 2019 |archive-url=https://web.archive.org/web/20190823203510/http://www.daviddarling.info/encyclopedia/L/line_of_nodes.html |url-status=live }} here they may be 'seen' as the points where the blue section of an orbit meets the pink.

Image:Inner Planet Orbits 02.svg|The perihelion (green) and aphelion (orange) points of the inner planets of the Solar System

Image:Outer Planet Orbits 02.svg|The perihelion (green) and aphelion (orange) points of the outer planets of the Solar System

The chart shows the extreme range—from the closest approach (perihelion) to farthest point (aphelion)—of several orbiting celestial bodies of the Solar System: the planets, the known dwarf planets, including Ceres, and Halley's Comet. The length of the horizontal bars correspond to the extreme range of the orbit of the indicated body around the Sun. These extreme distances (between perihelion and aphelion) are the lines of apsides of the orbits of various objects around a host body.

{{Distance from Sun using EasyTimeline}}

Currently, the Earth reaches perihelion in early January, approximately 14 days after the December solstice. At perihelion, the Earth's center is about {{val|0.98329}} astronomical units (AU) or {{convert|147098070|km|mi|abbr=on}} 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 {{val|1.01671|u=AU}} or {{convert|152097700|km|mi|abbr=on}}.

The dates of perihelion and aphelion change over time due to precession and other orbital factors, which follow cyclical patterns known as Milankovitch cycles. In the short term, such dates can vary up to 2 days from one year to another.{{cite web |url=https://www.timeanddate.com/astronomy/perihelion-aphelion-solstice.html |title=Perihelion, Aphelion and the Solstices |publisher=timeanddate.com |access-date=January 10, 2018 |archive-date=January 3, 2018 |archive-url=https://web.archive.org/web/20180103052358/https://www.timeanddate.com/astronomy/perihelion-aphelion-solstice.html |url-status=live }} 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 {{convert|4700|km|mi|-2}} 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).{{cite web |url=http://aa.usno.navy.mil/faq/docs/apsides.php |title=Variation in Times of Perihelion and Aphelion |publisher=Astronomical Applications Department of the U.S. Naval Observatory |date=August 11, 2011 |access-date=January 10, 2018 |archive-date=January 11, 2018 |archive-url=https://web.archive.org/web/20180111165154/http://aa.usno.navy.mil/faq/docs/apsides.php |url-status=dead }}

Because of the increased distance at aphelion, only 93.55% of the radiation from the Sun falls on a given area of Earth's surface as does at perihelion, but this does not account for the seasons, which result instead from the tilt of Earth's axis of 23.4° away from perpendicular to the plane of Earth's orbit.{{cite web|title=Solar System Exploration: Science & Technology: Science Features: Weather, Weather, Everywhere?|url=http://www.nasa.gov/audience/foreducators/postsecondary/features/F_Planet_Seasons.html|publisher=NASA|access-date=September 19, 2015|archive-date=September 29, 2015|archive-url=https://web.archive.org/web/20150929033150/http://www.nasa.gov/audience/foreducators/postsecondary/features/F_Planet_Seasons.html|url-status=live}} Indeed, at both perihelion and aphelion it is summer in one hemisphere while it is winter in the other one. 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, when solar radiation is lowest. Despite this, summers in the northern hemisphere are on average {{convert|2.3|C-change|F-change|0}} warmer than in the southern hemisphere, because the northern hemisphere contains larger land masses, which are easier to heat than the seas.{{cite web |url=http://spaceweather.com/glossary/aphelion.html |title=Earth at Aphelion |publisher=Space Weather |date=July 2008 |access-date=July 7, 2015 |archive-date=July 17, 2015 |archive-url=https://web.archive.org/web/20150717184242/http://spaceweather.com/glossary/aphelion.html |url-status=live }}

Perihelion and aphelion do however have an indirect effect on the seasons: because Earth's orbital speed is minimum at aphelion and maximum at perihelion, the planet takes longer to orbit from June solstice to September equinox than it does from December solstice to March equinox. Therefore, summer in the northern hemisphere lasts slightly longer (93 days) than summer in the southern hemisphere (89 days).{{cite web |last1=Rockport |first1=Steve C. |title=How much does aphelion affect our weather? We're at aphelion in the summer. Would our summers be warmer if we were at perihelion, instead? |url=https://usm.maine.edu/planet/how-much-does-aphelion-affect-our-weather-were-aphelion-summer-would-our-summers-be-warmer-if |website=Planetarium |publisher=University of Southern Maine |access-date=4 July 2020 |archive-date=July 6, 2020 |archive-url=https://web.archive.org/web/20200706154815/https://usm.maine.edu/planet/how-much-does-aphelion-affect-our-weather-were-aphelion-summer-would-our-summers-be-warmer-if |url-status=live }}

Astronomers commonly express the timing of perihelion relative to the First Point of Aries 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 2010, this had advanced by a small fraction of a degree to about 283.067°,{{cite web|url=http://data.giss.nasa.gov/ar5/srorbpar.html|archive-url=https://web.archive.org/web/20151002065753/http://data.giss.nasa.gov/ar5/srorbpar.html|archive-date=2015-10-02|title=Data.GISS: Earth's Orbital Parameters|website=data.giss.nasa.gov}} i.e. a mean increase of 62" per year.

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 (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, called the apsidal precession. (This is closely related to the precession of the axes.) The dates and times of the perihelions and aphelions for several past and future years are listed in the following table:{{Cite web|url=http://astropixels.com/ephemeris/perap2001.html|title=Earth at Perihelion and Aphelion: 2001 to 2100|last=Espenak|first=Fred|website=astropixels|access-date=June 24, 2021|archive-date=July 13, 2021|archive-url=https://web.archive.org/web/20210713131143/http://astropixels.com/ephemeris/perap2001.html|url-status=live}}

The following table shows the distances of the planets and dwarf planets from the Sun at their perihelion and aphelion.{{Cite web |url=http://solarsystem.nasa.gov/planets/compare |title=NASA planetary comparison chart |access-date=August 4, 2016 |archive-url=https://web.archive.org/web/20160804162808/http://solarsystem.nasa.gov/planets/compare |archive-date=August 4, 2016 }}

These formulae characterize the pericenter and apocenter of an orbit:

; Pericenter: Maximum speed, $v\_\backslash text\{per\}\; =\; \backslash sqrt\{\; \backslash frac\{(1\; +\; e)\backslash mu\}\{(1\; -\; e)a\}\; \}\; \backslash ,$, at minimum (pericenter) distance, $r\_\backslash text\{per\}\; =\; (1\; -\; e)a$.

; Apocenter: Minimum speed, $v\_\backslash text\{ap\}\; =\; \backslash sqrt\{\backslash frac\{(1\; -\; e)\backslash mu\}\{(1\; +\; e)a\}\; \}\; \backslash ,$, at maximum (apocenter) distance, $r\_\backslash text\{ap\}\; =\; (1\; +\; e)a$.

While, in accordance with Kepler's laws of planetary motion (based on the conservation of angular momentum) and the conservation of energy, these two quantities are constant for a given orbit:

; Specific relative angular momentum: $h\; =\; \backslash sqrt\{\backslash left(1\; -\; e^2\backslash right)\backslash mu\; a\}$

; Specific orbital energy: $\backslash varepsilon\; =\; -\backslash frac\{\backslash mu\}\{2a\}$

where:

• $r\_\backslash text\{ap\}$ is the distance from the apocenter to the primary focus
• $r\_\backslash text\{per\}$ is the distance from the pericenter to the primary focus
• a is the semi-major axis:
• : $a\; =\; \backslash frac\{r\_\backslash text\{per\}\; +\; r\_\backslash text\{ap\}\}\{2\}$
• μ is the standard gravitational parameter
• e is the eccentricity, defined as
• : $e\; =\; \backslash frac\{r\_\backslash text\{ap\}\; -\; r\_\backslash text\{per\}\}\{r\_\backslash text\{ap\}\; +\; r\_\backslash text\{per\}\}\; =\; 1\; -\; \backslash frac\{2\}\{\backslash frac\{r\_\backslash text\{ap\}\}\{r\_\backslash text\{per\}\}\; +\; 1\}$

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 arithmetic mean of the two limiting distances is the length of the semi-major axis a. The geometric mean of the two distances is the length of the semi-minor axis b.

The geometric mean of the two limiting speeds is

:$\backslash sqrt\{-2\backslash varepsilon\}\; =\; \backslash sqrt\{\backslash frac\{\backslash mu\}\{a\}\}$

which is the speed of a body in a circular orbit whose radius is $a$.

Orbital elements such as the time of perihelion passage are defined at the epoch chosen using an unperturbed two-body solution that does not account for the n-body problem. To get an accurate time of perihelion passage you need to use an epoch close to the perihelion passage. For example, using an epoch of 1996, Comet Hale–Bopp shows perihelion on 1 April 1997.{{Cite web |url=https://ssd.jpl.nasa.gov/sbdb.cgi?soln=J971A%2F1&sstr=Hale-Bopp&cad=1 |title=JPL SBDB: Hale-Bopp (Epoch 1996) |access-date=July 16, 2020 |archive-date=July 16, 2020 |archive-url=https://web.archive.org/web/20200716170854/https://ssd.jpl.nasa.gov/sbdb.cgi?soln=J971A%2F1&sstr=Hale-Bopp&cad=1 |url-status=live }} Using an epoch of 2008 shows a less accurate perihelion date of 30 March 1997.{{Cite web |url=https://ssd.jpl.nasa.gov/sbdb.cgi?sstr=1995O1 |title=JPL SBDB: Hale-Bopp |access-date=July 16, 2020 |archive-date=July 17, 2020 |archive-url=https://web.archive.org/web/20200717063814/https://ssd.jpl.nasa.gov/sbdb.cgi?sstr=1995O1 |url-status=live }} Short-period comets can be even more sensitive to the epoch selected. Using an epoch of 2005 shows 101P/Chernykh coming to perihelion on 25 December 2005,{{Cite web |url=http://www.oaa.gr.jp/~oaacs/nk/nk1293.htm |title=101P/Chernykh – A (NK 1293) by Syuichi Nakano |access-date=July 17, 2020 |archive-date=October 3, 2020 |archive-url=https://web.archive.org/web/20201003194829/http://www.oaa.gr.jp/~oaacs/nk/nk1293.htm |url-status=live }} but using an epoch of 2012 produces a less accurate unperturbed perihelion date of 20 January 2006.[https://web.archive.org/web/20201128092431/https://ssd.jpl.nasa.gov/sbdb.cgi?ID=c00101_0 JPL SBDB: 101P/Chernykh (Epoch 2012)]

{{anchor|12P}}

Numerical integration shows dwarf planet Eris will come to perihelion around December 2257.{{cite web

|title = Horizons Batch for Eris at perihelion around 7 December 2257 ±2 weeks

|type = Perihelion occurs when rdot flips from negative to positive. The JPL SBDB generically (incorrectly) lists an unperturbed two-body perihelion date in 2260

|url = https://ssd.jpl.nasa.gov/horizons_batch.cgi?batch=1&COMMAND=%27Eris%27&START_TIME=%272257-11-28%27&STOP_TIME=%272257-12-17%27&STEP_SIZE=%273%20hours%27&QUANTITIES=%2719%27

|work = JPL Horizons

|publisher = Jet Propulsion Laboratory

|access-date = 13 September 2021

|archive-date = September 13, 2021

|archive-url = https://web.archive.org/web/20210913110143/https://ssd.jpl.nasa.gov/horizons_batch.cgi?batch=1&COMMAND=%27Eris%27&START_TIME=%272257-11-28%27&STOP_TIME=%272257-12-17%27&STEP_SIZE=%273%20hours%27&QUANTITIES=%2719%27

|url-status = live

}} Using an epoch of 2021, which is 236 years early, less accurately shows Eris coming to perihelion in 2260.{{Cite web |url=https://ssd.jpl.nasa.gov/sbdb.cgi?sstr=Eris |title=JPL SBDB: Eris (Epoch 2021) |access-date=January 5, 2021 |archive-date=January 31, 2018 |archive-url=https://web.archive.org/web/20180131234951/https://ssd.jpl.nasa.gov/sbdb.cgi?sstr=Eris |url-status=live }}

4 Vesta came to perihelion on 26 December 2021,{{cite web

|title=Horizons Batch for 4 Vesta on 2021-Dec-26

|publisher=JPL Horizons

|type=Perihelion occurs when rdot flips from negative to positive

|url=https://ssd.jpl.nasa.gov/horizons_batch.cgi?batch=1&COMMAND=%27Vesta%27&START_TIME=%272021-Dec-25%2023:00%27&STOP_TIME=%272021-Dec-26%2004:00%27&STEP_SIZE=%2715%20minutes%27&QUANTITIES=%2719%27

|access-date=2021-09-26

|archive-date=September 26, 2021

|archive-url=https://web.archive.org/web/20210926095954/https://ssd.jpl.nasa.gov/horizons_batch.cgi?batch=1&COMMAND=%27Vesta%27&START_TIME=%272021-Dec-25%2023%3A00%27&STOP_TIME=%272021-Dec-26%2004%3A00%27&STEP_SIZE=%2715%20minutes%27&QUANTITIES=%2719%27

|url-status=live

}} (Epoch 2021-Jul-01/Soln.date: 2021-Apr-13) but using a two-body solution at an epoch of July 2021 less accurately shows Vesta came to perihelion on 25 December 2021.[https://web.archive.org/web/20210926095422/https://ssd.jpl.nasa.gov/sbdb.cgi?sstr=4 JPL SBDB: 4 Vesta (Epoch 2021)]

Trans-Neptunian objects discovered when 80+ AU from the Sun need dozens of observations over multiple years to well constrain their orbits because they move very slowly against the background stars. Due to statistics of small numbers, trans-Neptunian objects such as {{mpl|2015 TH|367}} when it had only 8 observations over an observation arc of 1 year that have not or will not come to perihelion for roughly 100 years can have a 1-sigma uncertainty of {{Convert|28220|day|year|order=flip|abbr=off}} in the perihelion date.{{Cite web |url=https://ssd.jpl.nasa.gov/sbdb.cgi?sstr=2015TH367 |title=JPL SBDB: 2015 TH367 |access-date=September 23, 2021 |archive-date=March 14, 2018 |archive-url=https://web.archive.org/web/20180314133928/https://ssd.jpl.nasa.gov/sbdb.cgi?sstr=2015TH367 |url-status=bot: unknown }}

• Distance of closest approach
• Eccentric anomaly
• Flyby (spaceflight)
• {{slink|Hyperbolic trajectory#Closest approach}}
• Mean anomaly
• Perifocal coordinate system
• True anomaly

{{reflist}}

{{Wiktionary|apsis}}

• [http://www.perseus.gr/Astro-Lunar-Scenes-Apo-Perigee.htm Apogee – Perigee] Photographic Size Comparison, perseus.gr
• [http://www.perseus.gr/Astro-Solar-Scenes-Aph-Perihelion.htm Aphelion – Perihelion] Photographic Size Comparison, perseus.gr
• [http://aa.usno.navy.mil/data/docs/EarthSeasons.php Earth's Seasons: Equinoxes, Solstices, Perihelion, and Aphelion, 2000–2020] {{Webarchive|url=https://web.archive.org/web/20071013000301/http://aa.usno.navy.mil/data/docs/EarthSeasons.php |date=October 13, 2007 }}, usno.navy.mil
• [http://aa.usno.navy.mil/data/docs/EarthSeasons.php Dates and times of Earth's perihelion and aphelion, 2000–2025] {{Webarchive|url=https://web.archive.org/web/20071013000301/http://aa.usno.navy.mil/data/docs/EarthSeasons.php |date=October 13, 2007 }} from the United States Naval Observatory
• [https://newton.spacedys.com/astdys/index.php?pc=3.2.1&pc0=3.2&udfs=0.3 List of asteroids currently closer to the Sun than Mercury] (These objects will be close to perihelion)
• JPL SBDB [https://ssd.jpl.nasa.gov/sbdb_query.cgi?obj_group=all;obj_kind=all;obj_numbered=all;ast_orbit_class=MBA;OBJ_field=0;ORB_field=0;c1_group=OBJ;c1_item=Ai;c1_op=%3C;c1_value=8;table_format=HTML;max_rows=200;format_option=comp;c_fields=AcBhBgBjBiBnBsAiBq;.cgifields=format_option;.cgifields=obj_kind;.cgifields=obj_group;.cgifields=obj_numbered;.cgifields=ast_orbit_class;.cgifields=table_format;.cgifields=com_orbit_class&query=1&c_sort=BqA list of Main-Belt Asteroids (H<8) sorted by perihelion date]

{{orbits}}

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Category:Orbits