APOGEEUSB - Apogee Instruments, Inc. Compatible Computer Devices

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Apogee|Perigeedate=July 2020thumb|345px|The apsides refer to the farthest (1) and nearest (2) points reached by an orbiting planetary body (1 and 2) with respect to a [[primary (astronomy)|primary, or host, body (3).*The line of apsides is the line connecting positions 1 and 2.*The table names the (two) apsides of a planetary body (X, "orbiter") orbiting the host body indicated: aligned table |cols=4 |style=width: 90%; text-align: left; font-size: normal; margin-left: 20; |row1header=y |(1) farthest |(X) orbiter |(3) host |(2) nearest |apogee |Moon |Earth |perigee |apojove |Ganymede |Jupiter |perijove |aphelion |Earth |Sun |perihelion |aphelion |Jupiter |Sun |perihelion |aphelion |Halley's Comet |Sun |perihelion |apastron |exoplanet |star |periastron |apocenter |comet, e.g. |primary |pericenter |apoapsis |comet, e.g. |primary |periapsis ____________________________________ For example, the Moon's two apsides are the farthest point, apogee, and the nearest point, perigee, of its orbit around the host Earth. The Earth's two apsides are the farthest point, aphelion, and the nearest point, perihelion, of its orbit around the host Sun. The terms aphelion and perihelion apply in the same way to the orbits of Jupiter and the other planets, the comets, and the asteroids of the Solar System. ]] thumb|upright=1.15|The two-body system of interacting elliptic orbits: The smaller, satellite body (blue) orbits the [[primary (astronomy)|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.]] thumb|upright=1.15|[[Kepler orbit|Keplerian orbital elements: point F, 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.]] plural apsides Greek: ἀψῖδες; "orbit") denotes either of the two extreme points (i.e., the farthest or nearest point) in the orbit of a planetary body about its primary body (or simply, "the primary"). The plural term, "apsides," usually implies both apsis points (i.e., farthest and nearest); apsides can also refer to the distance of the extreme range of an object orbiting a host body. For example, the apsides of Earth's orbit of the Sun are two: the apsis for Earth's farthest point from the Sun, dubbed the aphelion; and the apsis for Earth's nearest point, the perihelion (see top figure). (The term "apsis", a cognate with apse, comes via Latin from Greek). There are two apsides in any elliptic orbit. Each is named by selecting the appropriate prefix: ap-, apo- (|ἀπ(ό), (ap(o)-)|away from), or peri- (|περί (peri-)|near)-then joining it to the reference suffix of the "host" body being orbited. (For example, the reference suffix for Earth is -gee, hence apogee and perigee are the names of the apsides for the Moon, and any other artificial satellites of the Earth. The suffix for the Sun is -helion, hence aphelion and perihelion are the names of the apsides for the Earth and for the Sun's other planets, comets, asteroids, etc., (see table, top figure).) According to Newton's laws of motion all periodic orbits are ellipses, including: 1) the single orbital ellipse, where the primary body is fixed at one focus point and the planetary body orbits around that focus (see top figure); and 2) the two-body system of interacting elliptic orbits: both bodies orbit their joint center of mass (or barycenter), which is located at a focus point that is common to both ellipses, (see second figure). For such a two-body system, when one mass is sufficiently larger than the other, the smaller ellipse (of the larger body) around the barycenter comprises one of the orbital elements of the larger ellipse (of the smaller body). 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 barycenters of the central body and 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).