Apsis

s: 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- () for the farthest or peri- () 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. 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). 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. ==Terminology==

The words "pericenter" and "apocenter" are often seen, although periapsis and 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 (), and the point of greatest distance is the aphelion (); 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 (), and of greatest distance, the apogee (from Ancient Greek: Γῆ (Gē), "land" or "earth"). • For objects in lunar orbit, the point of least distance are called the pericynthion () and the greatest distance the apocynthion (). The terms perilune and apolune, as well as periselene and aposelene are also used. 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). More recently, during the Artemis program, the terms perilune and apolune have been used. Regarding black holes, the term peribothron was first used in a 1976 paper by J. Frank and M. J. Rees, 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, thus appearing before perinigricon and aponigricon (from Latin) in the scientific literature in 2002. Terminology summary 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. ==Perihelion and aphelion==

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. Inner planets and outer planets The two images below show the orbits, orbital nodes, and positions of perihelion (q) and aphelion (Q) for the planets of the Solar System 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; 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 Lines of apsides 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. Earth perihelion and aphelion In the 21st century, the Earth reaches perihelion in early January, approximately 14 days after the December solstice. At perihelion, the Earth's center is about The dates of perihelion and aphelion change over a century 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 3 days from one year to another as with aphelion on 3 July 2025 and 6 July 2026. This short-term 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 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). On a longer time scale, the last July 3 aphelion is in 2060, and the last January 2 perihelion is in 2089. 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 warmer than in the southern hemisphere, because the northern hemisphere contains larger land masses, which are easier to heat than the seas. 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). 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°, 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 perihelion and of aphelion progress through the seasons, and they make one complete cycle in 22,000 to 26,000 years. By the year 3800, perihelion will regularly occur in February. Other planets The following table shows the distances of the planets and dwarf planets from the Sun at their perihelion and aphelion. ==Mathematical formulae==

These formulae characterize the pericenter and apocenter of an orbit: ; Pericenter: Maximum speed, v_\text{per} = \sqrt{ \frac{(1 + e)\mu}{(1 - e)a} } \,, at minimum (pericenter) distance, r_\text{per} = (1 - e)a. ; Apocenter: Minimum speed, v_\text{ap} = \sqrt{\frac{(1 - e)\mu}{(1 + e)a} } \,, at maximum (apocenter) distance, r_\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 = \sqrt{\left(1 - e^2\right)\mu a} ; Specific orbital energy: \varepsilon = -\frac{\mu}{2a} where: • r_\text{ap} is the distance from the apocenter to the primary focus • r_\text{per} is the distance from the pericenter to the primary focus • a is the semi-major axis: • : a = \frac{r_\text{per} + r_\text{ap}}{2} • μ is the standard gravitational parameter • e is the eccentricity, defined as • : e = \frac{r_\text{ap} - r_\text{per}}{r_\text{ap} + r_\text{per}} = 1 - \frac{2}{\frac{r_\text{ap}}{r_\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 :\sqrt{-2\varepsilon} = \sqrt{\frac{\mu}{a}} which is the speed of a body in a circular orbit whose radius is a. == Time of perihelion ==

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. Using an epoch of 2022 shows a less accurate perihelion date of 29 March 1997. 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, but using an epoch of 2012 produces a less accurate unperturbed perihelion date of 20 January 2006. Numerical integration shows dwarf planet Eris will come to perihelion around December 2257. Using an epoch of 2025 less accurately shows Eris coming to perihelion in August 2257. 4 Vesta came to perihelion on 26 December 2021, but using a two-body solution at an epoch of July 2021 less accurately shows Vesta came to perihelion on 25 December 2021. Short observation periods Trans-Neptunian objects that are discovered when they are more than 80 AU from the Sun present a major challenge for astronomers. Because these objects move extremely slowly across the sky, scientists need many observations taken over several years to accurately determine their orbital paths. When astronomers have only limited data—like when there were only 8 observations of object collected over just one year—the uncertainty becomes enormous. For objects that won’t reach their closest point to the Sun (perihelion) for roughly 100 years, this limited data can lead to massive uncertainties. In the case of , scientists originally estimated the perihelion date could be off by plus or minus (a 1-sigma uncertainty) —that’s nearly an entire human lifetime of uncertainty. This demonstrates why tracking these distant objects requires patience and long-term observation campaigns to pin down their true orbital characteristics. ==See also==