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Orbital elements are the parameters required to uniquely identify a specific orbit. In celestial mechanics these elements are considered in two-body systems using a Kepler orbit. There are many different ways to mathematically describe the same orbit, but certain schemes are commonly used in astronomy and orbital mechanics.

A real orbit and its elements change over time due to gravitational perturbations by other objects and the effects of general relativity. A Kepler orbit is an idealized, mathematical approximation of the orbit at a particular time.

When viewed from an inertial frame, two orbiting bodies trace out distinct trajectories. Each of these trajectories has its focus at the common center of mass. When viewed from a non-inertial frame centered on one of the bodies, only the trajectory of the opposite body is apparent; Keplerian elements describe these non-inertial trajectories. An orbit has two sets of Keplerian elements depending on which body is used as the point of reference. The reference body (usually the most massive) is called the primary, the other body is called the secondary. The primary does not necessarily possess more mass than the secondary, and even when the bodies are of equal mass, the orbital elements depend on the choice of the primary.

Orbital elements can be obtained from orbital state vectors (position and velocity vectors along with time and magnitude of acceleration) by manual transformations or with computer software through a process known as orbit determination.^[1]

It non-closed orbits exist, although these are typically referred to as trajectories and not orbits, as they are not periodic. The same elements used to describe closed orbits can also typically be used to represent open trajectories.

Common orbital elements by type

Required parameters

In general, eight parameters are necessary to unambiguously define an arbitrary and unperturbed orbit. This is because the problem contains eight degrees of freedom. These correspond to the three spatial dimensions which define position ( $x$ , $y$ , $z$ in a Cartesian coordinate system), the velocity in each of these dimensions, the magnitude of acceleration (only magnitude is needed, as the direction is always opposite the position vector), and the current time (epoch). The mass or standard gravitational parameter of the central body can specified instead of the acceleration, as one can be used to find the other given the position vector through the relation $a=\mu /r^{2}$ . These parameters can be described as orbital state vectors, but this is often an inconvenient and opaque way to represent an orbit, which is why orbital elements are commonly used instead.

When describing an orbit with orbital elements, typically two are needed to describe the size and shape of the trajectory, three are needed describe the rotation of the orbit, one is needed to describe the speed of motion, and two elements are needed to describe the position of the body around its orbit along with the epoch time at which this occurs. However, if the epoch time is chosen to be the time at which the position-describing element of choice (e.g. mean anomaly) is equal to some constant (usually zero), then said element can be omitted, meaning only seven elements are required in total.

Commonly only 6 variables are specified for a given orbit, as the motion-describing variable can be the mass or standard gravitational parameter of the central body, which is often already known and does not need specifying, and the epoch time can be considered part of the reference frame and not as a distinct element. However, in any case, 8 values will need to be known, regardless of how they are categorized.

Additionally, certain elements can be omitted if they are not required for the desired application (e.g. both epoch elements and the motion element are not needed if only the shape and orientation need to be known).

Size and shape describing parameters

Two parameters are required to describe the size and the shape of an orbit. Generally any two of these values can be used to calculate any other (as described below), so the choice of which to use is one of preference and the particular use case.

Eccentricity ( $e$ ) — shape of the ellipse, describing how much it deviates from a perfect a circle. An eccentricity of zero describes a perfect circle, values less than 1 describe an ellipse, values greater than 1 describe a hyperbolic trajectory, and a value of exactly 1 describes a parabola.^[2]
Semi-major axis ( $a$ ) — half the distance between the apoapsis and periapsis (long axis of the ellipse). This value is positive for elliptical orbits, infinity for parabolic trajectories, and negative for hyperbolic trajectories, which can hinder it's usability when working with different types of trajectories.^[3]
Semi-minor axis ( $b$ ) — half the short axis of the ellipse. This value shares the same limitations as with the semi-major axis.
Semi-parameter ( $p$ ) — the width of the orbit at the primary focus (at a true anomaly of $π/2$ or 90°). This value is useful for it's use in the orbit equation, which can return the distance from the central body given $p$ and the true anomaly for any type of orbit or trajectory. This value is also commonly referred to as the semi-latus rectum, and given the symbol $ℓ$ . Additionally, this value will always be defined and positive unlike the semi-major and semi-minor axes.^[3]
Apoapsis ( $r a$ ) — The farthest point in the orbit from the central body (at a true anomaly of $π$ or 180°). This quantity is undefined (or infinity) for parabolic and hyperbolic trajectories, as they continue moving away from the central body forever. This value is sometimes given the symbol $Q$ .^[2]
Periapsis ( $r p$ ) — The closest point in the orbit from the central body (at a true anomaly of 0). Unlike with apoapsis, this quantity is defined for all orbit types. This value is sometimes given the symbol $q$ .^[2]

It is worth mentioning that for perfectly circular orbits, there are no points on the orbit that can be described as either the apoapsis or periapsis, as they all have the same distance from the central body. Additionally it is common to see the affix for apoapsis and periapsis changed depending on the central body (e.g. apogee and perigee for orbits of the Earth, and aphelion and perihelion for orbits of the Sun).

Other parameters can also be used to describe the size and shape of an orbit such as the linear eccentricity, flattening, and focal parameter, but the use of these is limited.

Relations between elements

This section contains the common relations between these orbital elements, but more relations can be derived through manipulations of one or more of these equations. The variable names used here are consistent with the ones described above.

Eccentricity can be found using the semi-minor and semi-major axes like so:
$e={\sqrt {1-{\frac {b^{2}}{a^{2}}}}}$ when $a>0$ , $e={\sqrt {1+{\frac {b^{2}}{a^{2}}}}}$ when $a<0$

Eccentricity can also be found using the apoapsis and periapsis through this relation:
$e={\frac {r_{a}-r_{p}}{r_{a}+r_{p}}}$

The semi-major axis can be found using the fact that the line that connects the apoapsis to the center of the conic, and from the center to the periapsis both combined span the length of the conic, and thus the major axis. This is then divided by 2 to get the semi-major axis.
$a={\frac {r_{p}+r_{a}}{2}}$

The semi-minor axis can be found using the semi-major axis and eccentricity through the following relations. Two formula are needed to avoid taking the square root of a negative number.
$b=a{\sqrt {1-e^{2}}}$ when $e<1$ , $b=a{\sqrt {e^{2}-1}}$ when $e>1$

The semi-parameter can be found using the semi-major axis and eccentricity like so:
$p=a\left(1-e^{2}\right)$

Apoapsis can be found using the following equation, which is a form of the orbit equation solved for $\nu =\pi$ .
$r_{a}={\frac {p}{1-e}}$ , when $e<1$

Periapsis can be found using the following equation, which, as with the equation for apoapsis, is a form of the orbit equation instead solved for $\nu =0$ .
$r_{p}={\frac {p}{1+e}}$

Rotation describing elements

In this diagram, the orbital plane (yellow) intersects a reference plane (gray). For Earth-orbiting satellites, the reference plane is usually the Earth's equatorial plane, and for satellites in solar orbits it is the ecliptic plane. The intersection is called the line of nodes, as it connects the reference body (the primary) with the ascending and descending nodes. The reference body and the vernal point (♈︎) establish a reference direction and, together with the reference plane, they establish a reference frame.

Three parameters are required to describe the orientation of the plane of the orbit, and the orientation of the orbit within that plane.

Inclination ( $i$ ) — vertical tilt of the ellipse with respect to the reference plane, typically the equator of the central body, measured at the ascending node (where the orbit passes crosses the reference plane, represented by the green angle $i$ in the diagram). Inclinations near zero indicate equatorial orbits, and inclinations near 90° indicate polar orbits. Inclinations from 90-180° are typically used to denote retrograde orbits.
Longitude of the ascending node ( $Ω$ ) — describes the angle from the ascending node of the orbit ( $☊$ in the diagram) to the reference frame's reference direction (♈︎ in the diagram). This is measured in the reference plane, and is shown as the green angle $Ω$ in the diagram. This quantity is undefined for perfectly equatorial (coplanar) orbits, but is often set to zero instead by convention.^[3] This quantity is also sometimes referred to as the right ascension of the ascending node (or RAAN).
Argument of periapsis ( $ω$ ) — defines the orientation of the ellipse in the orbital plane, as an angle measured from the ascending node to the periapsis (the closest point the satellite body comes to the primary body around which it orbits), the purple angle $ω$ in the diagram. This quantity is undefined for circular orbits, but is often set to zero instead by convention.^[3]

These three elements together can be described as Euler angles defining the orientation of the orbit relative to the reference coordinate system. Although these three are the most common, other elements do exist, and are useful to describe other properties of the orbit.

Longitude of periapsis ( $ϖ$ ) — describes the angle between the vernal point and the periapsis, measured in the reference plane. This can be described as the sum of the longitude of the ascending node and the argument of periapsis: $\varpi =\Omega +\omega$ . Unlike the longitude of the ascending node, this value is defined for orbits where the inclination is zero.

Motion over time describing elements

One parameter is required to describe the speed of motion of the orbiting object around the central body. However, this can be omitted if only a description of the shape of the orbit is required. Various quantities that do not directly describe a speed can be used to satisfy this condition, and it is possible to convert from one to any other (formula below).

Mean motion ( $n$ ) — quantity that describes the average angular speed of the orbiting body, measured as an angle per unit time. For non-circular orbits, the actual angular speed is not constant, so the mean motion will not describe a physical angle. Instead this corresponds to a change in the mean anomaly, which indeed increases linearly with time.
Orbital period ( $P$ ) — the time it takes for the orbiting body to complete one full revolution around the central body. This quantity is undefined for parabolic and hyperbolic trajectories, as they are non-periodic.
Standard gravitational parameter ( $μ$ ) — quantity equal to the mass of the central body times the gravitational constant $G$ . This quantity is often used instead of mass, as it can be easier to measure with precision than either mass or $G$ , and will need to be calculated in any case in order to find the acceleration due to gravity. This is also often not included as part of orbital element lists, as it can assumed to be known based on the central body.
Mass of the central body ( $M$ ) — the mass of only the central body can be used, as in most cases the mass of the orbiting body is insignificant and does not meaningfully influence the trajectory. However, when this is not the case (e.g. binary stars), the mass of the 2-body system can be used instead.

Relations between elements

This section contains the common relations between the set of orbital elements described above, but more relations can be derived through manipulations of one or more of these equations. The variable names used here are consistent with the ones described above.

Mean motion can be calculated using the standard gravitational parameter and the semi-major axis of the orbit ( $μ$ can be substituted for $GM$ ). This equation returns the mean motion in radians, and will need to be converted if $n$ is desired to be in a different unit.
$n={\sqrt {\frac {\mu }{a^{3}}}}$ when $a>0$ , $n={\sqrt {\frac {\mu }{-a^{3}}}}$ when $a<0$

It is worth noting that because the semi-major axis is related to the mean motion and standard gravitational parameter, it can be calculated without being specified. This is especially useful if $μ$ is assumed to be known, as then $n$ can be used to calculate $a$ , and likewise for specifying $a$ . This can allow one less element to specified.

Orbital period can be found from $n$ given the fact that the mean motion can be described as a frequency (number of orbits per unit time), which is the inverse of period.
$P={\frac {2\pi }{n}}$ if $n$ is in radians, or $P={\frac {360^{\circ }}{n}}$ if $n$ is in degrees.

The standard gravitational parameter can be found given the mean motion and the semi-major axis through the following relation (assuming that $n$ is in radians):
$\mu =n^{2}a^{3}$

The mass of the central body can be found given the standard gravitational parameter using a rearrangement of its definition as the product of the mass and the gravitational constant.
$M={\frac {\mu }{G}}$

Epoch describing elements

Two elements are needed to describe the position of the body around its orbit, and the time at which this occurs. If this time is defined to be at a point where the specific position variable is a designated constant (usually zero), then it does not need to be specified.

Epoch ( $t 0$ ) — time at which one of the below elements is defined. Alternatively this is the point in time where the orbital elements were measured. Sometimes the epoch time is considered as part of the reference frame and is not listed as a distinct element.
Time of periapsis passage ( $T 0$ ) — time at which the orbiting body is at periapsis. This is also when the mean anomaly and true anomaly (and others) are zero, so they do not need to be defined. This value is not defined for circular orbits, as they do not have a uniquely defined point of periapsis.
Mean anomaly at epoch ( $M 0$ ) — mean anomaly at the epoch time. Mean anomaly is a mathematically convenient angle that increases linearly with time as if the orbit were perfectly circular. Zero is defined as being at periapsis, and one period spans 2 $π$ radians. The rate at which the mean anomaly increases is equal to the mean motion $n$ . Because this angle is relative to periapsis, it is not defined for circular orbits.
Mean longitude at epoch ( $L 0$ ) — mean longitude at the epoch time. Mean longitude is similar to mean anomaly, in that it increases linearly with time and does not represent the real angular displacement. Unlike with mean anomaly, mean longitude is defined relative to the vernal point, which means it is defined for circular orbits.
Eccentric anomaly at epoch ( $E 0$ ) — the eccentric anomaly at the epoch time. Eccentric anomaly is defined at the angular displacement along the auxiliary circle of the ellipse (circle tangent to the ellipse both at apses). This value takes into account the varying speed of objects in elliptical orbits, but does not account for the elliptical shape of the orbit. As such, it still does not correspond to the real angular displacement of the orbiting body. Like with mean anomaly and true anomaly, the eccentric anomaly is measured relative to periapsis, and is not defined for circular orbits. The eccentric anomaly is also not defined for parabolic and hyperbolic trajectories, and instead the parabolic anomaly or hyperbolic anomaly are used.^[3]
True anomaly at epoch ( $\nu _{0}$ ) — angle that represents the real angular displacement of the orbiting body at the epoch time, taking into account the varying speed and elliptical shape of an orbit. Like with mean anomaly, true anomaly is measured relative to periapsis, and thus it has the same limitations with circular orbits.
True longitude at epoch ( $l 0$ ) — the angular displacement of the orbiting body at the epoch time. Unlike with the true anomaly, the true longitude is measured relative to the vernal point, so it can be defined for circular orbits.
Mean argument of latitude ( $u M0$ ) at epoch — the angular displacement of the orbiting body at the epoch time. Mean argument of latitude is similar to the mean anomaly and mean longitude, but instead it is measured relative to the ascending node. This means while it is well defined for circular orbits, it is not for equatorial orbits.^[3]
Argument of latitude at epoch ( $u 0$ ) — the angular displacement of the orbiting body at the epoch time. This angle is measured relative to the ascending node, so while it is defined for circular orbits, it is not defined for equatorial orbits.

It is worth mentioning that these elements are also used to describe the position of an object in it's orbit in a more general context, and are not limited to describing the state at an epoch time.

Relations between elements

This section contains the common relations between the set of orbital elements described above, but more relations can be derived through manipulations of one or more of these equations. The variable names used here are consistent with the ones described above. These formulae also hold true for conversions between these elements in general.

Epoch can be found given the time of periapsis passage, the mean anomaly at epoch, and mean motion like so:
$t_{0}=T_{0}+{\frac {M_{0}}{n}}$

Time of periapsis passage can be found from the epoch, mean anomaly at epoch, and mean motion by re-arranging the previous equation like so:
$T_{0}=t_{0}-{\frac {M_{0}}{n}}$

Mean anomaly can be found from the eccentric anomaly and eccentricity using Kepler's equation like so:
$M=E-e\sin E$

Mean longitude can be found using the mean anomaly at epoch and the longitude of periapsis.
$L=M+\varpi$ or $L=M+\omega +\Omega$

Eccentric anomaly can be found with the mean anomaly and eccentricity using Kepler's equation through various means, such as iterative calculations or numerical solutions (for some values of $e$ ). Kepler's equation is given as
$E=M+e\sin E$ ,

and can be solved through a root-finding algorithm (usually Newton's Method) like so:
$E_{n+1}=E_{n}+{\frac {M-E_{n}+e\sin(E_{n})}{1-e\cos(E_{n})}}$

Typically a starting guess of either $M$ , $M-e$ , $M+e$ , or $M+e\sin M$ are used.^[3]^[4] This iteration can be repeated until a desired level of tolerance is reached.

True anomaly can be found from the eccentric anomaly and through the following relations. The quadrant of the solution can be resolved using an atan2(y,x) function.^[3]
$\sin \nu ={\frac {{\sqrt {1-e^{2}}}\sin E}{1-e\cos \left(E\right)}},\cos \nu ={\frac {\cos E-e}{1-e\cos E}}$

True longitude can be found using the true anomaly and longitude of periapsis through the following relation:
$l=\nu +\varpi$ or $l=\nu +\omega +\Omega$

Mean argument of latitude can be calculated using the mean anomaly and argument of periapsis like so:
$u_{M}=\Omega +M$

Argument of latitude can be found using the true anomaly and argument of periapsis like so:
$u=\nu +\Omega$

Common sets of elements

Classical Keplerian elements

While in theory, any set of elements that meets the requirements above can be used to describe an orbit, in practice, certain sets are much more common than others.

The most common elements used to describe the size and shape of the orbit are the semi-major axis ( $a$ ), and the eccentricity ( $e$ ). Sometimes the semi-parameter ( $p$ ) is used instead of $a$ , as the semi-major axis is infinite for parabolic trajectories, and thus cannot be used. ^[3]^[2]

It is common to specify the period ( $P$ ) or mean motion ( $n$ ) instead of the semi-major axis in Keplerian element sets, as each can be computed from the other provided the standard gravitational parameter ( $\mu$ ) is known for the central body though the relations above.

For the epoch, the epoch time ( $t$ ) along with the mean anomaly ( $M 0$ ), mean longitude ( $L 0$ ), true anomaly ( $\nu _{0}$ ) or (rarely) the eccentric anomaly ( $E 0$ ) are often used. The time of periapsis passage ( $T 0$ ) is also sometimes used for this purpose.^[2]

It is also quite common to see either the mean anomaly or the mean longitude expressed directly, without either $M 0$ or $L 0$ as intermediary steps, as a linear function of time. This method of expression will consolidate the mean motion as the slope of this linear equation. An example of this is provided below:
$M(t)=M_{0}+n(t-t_{0})$

Elements by body type

The choice of elements can differ depending on the type of astronomical body. The eccentricity ( $e$ ) and either the semi-major axis ( $a$ ) or the distance of periapsis ( $q$ ) are used to specify the shape and size of an orbit. The longitude of the ascending node ( $Ω$ ) the inclination ( $i$ ) and the argument of periapsis ( $ω$ ) or the longitude of periapsis ( $ϖ$ ) specify the orientation of the orbit in its plane. Either the Mean longitude at epoch ( $L 0$ ) the mean anomaly at epoch ( $M 0$ ) or the time of periapsis passage ( $T 0$ ) are used to specify a known point in the orbit. The choices made depend whether the vernal equinox or the node are used as the primary reference.^[5]^[6]

Sets of orbital elements
Object	Elements used
Major planet	$e, a, i, Ω, ϖ, L 0$
Comet	$e, q, i, Ω, ω, T 0$
Asteroid	$e, a, i, Ω, ω, M 0$

Two-line elements

Orbital elements can be encoded as text in a number of formats. The most common of them is the NASA / NORAD "two-line elements" (TLE) format,^[7] originally designed for use with 80 column punched cards, but still in use because it is the most common format, and 80-character ASCII records can be handled efficiently by modern databases.

The two-line element format lists the eccentricity ( $e$ ), inclination ( $i$ ), longitude of the ascending node ( $Ω$ ), argument of periapsis ( $ω$ ), mean motion ( $n$ ), epoch ( $t 0$ ), and mean anomaly at epoch ( $M 0$ ).^[7]^[3] Since the format is primarily meant for orbits of the Earth, the standard gravitational parameter ( $μ$ ), can be assumed and used to calculate the semi-major axis with the mean motion via the relation above.

Depending on the application and object orbit, the data derived from TLEs older than 30 days can become unreliable. Orbital positions can be calculated from TLEs through simplified perturbation models (SGP4 / SDP4 / SGP8 / SDP8).^[8]

Example of a two-line element:^[9]

1 27651U 03004A   07083.49636287  .00000119  00000-0  30706-4 0  2692
2 27651 039.9951 132.2059 0025931 073.4582 286.9047 14.81909376225249

Delaunay variables

The Delaunay orbital elements were introduced by Charles-Eugène Delaunay during his study of the motion of the Moon.^[10] Commonly called Delaunay variables, they are a set of canonical variables, which are action-angle coordinates. The angles are simple sums of some of the Keplerian angles, and are often referred to with different symbols than other in applications like so:

the mean longitude: $\ell =L=M+\omega +\Omega$ ,
the longitude of periapsis: $g=\varpi =\omega +\Omega$ , and
the longitude of the ascending node: $h=\Omega$

along with their respective conjugate momenta, $L$ , $G$ , and $H$ .^[11] The momenta $L$ , $G$ , and $H$ are the action variables and are more elaborate combinations of the Keplerian elements $a$ , $e$ , and $i$ .

Delaunay variables are used to simplify perturbative calculations in celestial mechanics, for example while investigating the Kozai–Lidov oscillations in hierarchical triple systems.^[11] The advantage of the Delaunay variables is that they remain well defined and non-singular (except for $h$ , which can be tolerated) even for circular and equatorial orbits.

Euler angle transformations

The angles $Ω$ , $i$ , $ω$ are the Euler angles (corresponding to $α$ , $β$ , $γ$ in the notation used in that article) characterizing the orientation of the coordinate system

$x̂$ , $ŷ$ , $ẑ$ from the inertial coordinate frame $Î$ , $Ĵ$ , $K̂$

where:

$Î$ , $Ĵ$ is in the equatorial plane of the central body. $Î$ is in the direction of the vernal equinox. $Ĵ$ is perpendicular to $Î$ and with $Î$ defines the reference plane. $K̂$ is perpendicular to the reference plane. Orbital elements of bodies (planets, comets, asteroids, ...) in the Solar System usually the ecliptic as that plane.
$x̂$ , $ŷ$ are in the orbital plane and with $x̂$ in the direction to the pericenter (periapsis). $ẑ$ is perpendicular to the plane of the orbit. $ŷ$ is mutually perpendicular to $x̂$ and $ẑ$ .

Then, the transformation from the $Î$ , $Ĵ$ , $K̂$ coordinate frame to the $x̂$ , $ŷ$ , $ẑ$ frame with the Euler angles $Ω$ , $i$ , $ω$ is: ${\begin{aligned}x_{1}&=\cos \Omega \cdot \cos \omega -\sin \Omega \cdot \cos i\cdot \sin \omega \ ;\\x_{2}&=\sin \Omega \cdot \cos \omega +\cos \Omega \cdot \cos i\cdot \sin \omega \ ;\\x_{3}&=\sin i\cdot \sin \omega ;\\\,\\y_{1}&=-\cos \Omega \cdot \sin \omega -\sin \Omega \cdot \cos i\cdot \cos \omega \ ;\\y_{2}&=-\sin \Omega \cdot \sin \omega +\cos \Omega \cdot \cos i\cdot \cos \omega \ ;\\y_{3}&=\sin i\cdot \cos \omega \ ;\\\,\\z_{1}&=\sin i\cdot \sin \Omega \ ;\\z_{2}&=-\sin i\cdot \cos \Omega \ ;\\z_{3}&=\cos i\ ;\\\end{aligned}}$ ${\begin{bmatrix}x_{1}&x_{2}&x_{3}\\y_{1}&y_{2}&y_{3}\\z_{1}&z_{2}&z_{3}\end{bmatrix}}={\begin{bmatrix}\cos \omega &\sin \omega &0\\-\sin \omega &\cos \omega &0\\0&0&1\end{bmatrix}}\,{\begin{bmatrix}1&0&0\\0&\cos i&\sin i\\0&-\sin i&\cos i\end{bmatrix}}\,{\begin{bmatrix}\cos \Omega &\sin \Omega &0\\-\sin \Omega &\cos \Omega &0\\0&0&1\end{bmatrix}}\,;$ where ${\begin{aligned}\mathbf {\hat {x}} &=x_{1}\mathbf {\hat {I}} +x_{2}\mathbf {\hat {J}} +x_{3}\mathbf {\hat {K}} ~;\\\mathbf {\hat {y}} &=y_{1}\mathbf {\hat {I}} +y_{2}\mathbf {\hat {J}} +y_{3}\mathbf {\hat {K}} ~;\\\mathbf {\hat {z}} &=z_{1}\mathbf {\hat {I}} +z_{2}\mathbf {\hat {J}} +z_{3}\mathbf {\hat {K}} ~.\\\end{aligned}}$

The inverse transformation, which computes the 3 coordinates in the I-J-K system given the 3 (or 2) coordinates in the x-y-z system, is represented by the inverse matrix. According to the rules of matrix algebra, the inverse matrix of the product of the 3 rotation matrices is obtained by inverting the order of the three matrices and switching the signs of the three Euler angles.

That is,

${\begin{bmatrix}i_{1}&i_{2}&i_{3}\\j_{1}&j_{2}&j_{3}\\k_{1}&k_{2}&k_{3}\end{bmatrix}}={\begin{bmatrix}\cos \Omega &-\sin \Omega &0\\\sin \Omega &\cos \Omega &0\\0&0&1\end{bmatrix}}\,{\begin{bmatrix}1&0&0\\0&\cos i&-\sin i\\0&\sin i&\cos i\end{bmatrix}}\,{\begin{bmatrix}\cos \omega &-\sin \omega &0\\\sin \omega &\cos \omega &0\\0&0&1\end{bmatrix}}\,;$ where ${\begin{aligned}\mathbf {\hat {I}} &=i_{1}\mathbf {\hat {x}} +i_{2}\mathbf {\hat {y}} +i_{3}\mathbf {\hat {z}} ~;\\\mathbf {\hat {J}} &=j_{1}\mathbf {\hat {x}} +j_{2}\mathbf {\hat {y}} +j_{3}\mathbf {\hat {z}} ~;\\\mathbf {\hat {K}} &=k_{1}\mathbf {\hat {x}} +k_{2}\mathbf {\hat {y}} +k_{3}\mathbf {\hat {z}} ~.\\\end{aligned}}$

The transformation from $x̂$ , $ŷ$ , $ẑ$ to Euler angles $Ω$ , $i$ , $ω$ is: ${\begin{aligned}\Omega &=\operatorname {arg} \left(-z_{2},z_{1}\right)\\i&=\operatorname {arg} \left(z_{3},{\sqrt {{z_{1}}^{2}+{z_{2}}^{2}}}\right)\\\omega &=\operatorname {arg} \left(y_{3},x_{3}\right)\\\end{aligned}}$ where $arg(x, y)$ signifies the polar argument that can be computed with the standard function atan2(y,x) available in many programming languages.

Perturbations and elemental variance

Unperturbed, two-body, Newtonian orbits are always conic sections, so the Keplerian elements define an unchanging ellipse, parabola, or hyperbola. Real orbits have perturbations, so a given set of Keplerian elements accurately describes an orbit only at the epoch. Evolution of the orbital elements takes place due to the gravitational pull of bodies other than the primary, the non-sphericity of the primary, atmospheric drag, relativistic effects, radiation pressure, electromagnetic forces, and so on.

Keplerian elements can often be used to produce useful predictions at times near the epoch. Alternatively, real trajectories can be modeled as a sequence of Keplerian orbits that osculate ("kiss" or touch) the real trajectory. They can also be described by the so-called planetary equations, differential equations which come in different forms developed by Lagrange, Gauss, Delaunay, Poincaré, or Hill.

References

^ For example, with "VEC2TLE". amsat.org. Archived from the original on 20 May 2016. Retrieved 19 June 2013.
^ ^a ^b ^c ^d ^e Weber, Bryan. "Orbital Mechanics". Orbital Mechanics. "Orbital Nomenclature", and "Classical Orbital Elements". Retrieved 21 February 2025.{{cite web}}: CS1 maint: url-status (link)
^ ^a ^b ^c ^d ^e ^f ^g ^h ⁱ ^j Vallado, David A. (2022). Fundamentals of astrodynamics and applications. Space technology library (4th ed.). Torrance, CA: Microcosm Press. pp. 41–112. ISBN 978-1-881883-18-0.
^ Standish, E. Myles; Williams, James G. "Approximate Positions of the Planets". NASA Solar System Dynamics. Retrieved 20 February 2025.{{cite web}}: CS1 maint: url-status (link)
^ Green, Robin M. (1985). Spherical Astronomy. Cambridge University Press. ISBN 978-0-521-23988-2.
^ Danby, J. M. A. (1962). Fundamentals of Celestial Mechanics. Willmann-Bell. ISBN 978-0-943396-20-0.
^ ^a ^b Kelso, T.S. "FAQs: Two-line element set format". celestrak.com. CelesTrak. Archived from the original on 26 March 2016. Retrieved 15 June 2016.
^ Seidelmann, K.P., ed. (1992). Explanatory Supplement to the Astronomical Almanac (1st ed.). Mill Valley, CA: University Science Books.
^ "SORCE". Heavens-Above.com. orbit data. Archived from the original on 27 September 2007.
^ Aubin, David (2014). "Delaunay, Charles-Eugène". Biographical Encyclopedia of Astronomers. New York City: Springer New York. pp. 548–549. doi:10.1007/978-1-4419-9917-7_347. ISBN 978-1-4419-9916-0.
^ ^a ^b Shevchenko, Ivan (2017). The Lidov–Kozai effect: applications in exoplanet research and dynamical astronomy. Cham: Springer. ISBN 978-3-319-43522-0.

External links

Gurfil, Pini (2005). "Euler parameters as nonsingular orbital elements in Near-Equatorial Orbits". Journal of Guidance, Control, and Dynamics. 28 (5): 1079–1084. Bibcode:2005JGCD...28.1079G. doi:10.2514/1.14760.

"Tutorial". AMSAT. Keplerian elements. Archived from the original on 14 October 2002.
"Orbits Tutorial". marine.rutgers.edu. Archived from the original on 19 April 2021. Retrieved 30 July 2019.
"Orbital elements visualizer". orbitalmechanics.info.
Report No. 3 (PDF). celestrak (Report). Spacetrack. North American Aerospace Defense Command (NORAD). Archived (PDF) from the original on 3 September 2000. – a serious treatment of orbital elements
"FAQ". Celestrak. Two-Line Elements. Archived from the original on 26 March 2016.
"The JPL HORIZONS online ephemeris". – also furnishes orbital elements for a large number of solar system objects
"Mean orbital parameters". ssd.jpl.nasa.gov. Planetary satellites. JPL / NASA.
"Introduction to exporting". ssd.jpl.nasa.gov. JPL planetary and lunar ephemerides. JPL / NASA.
"State vectors: VEC2TLE". MindSpring (software). Archived from the original on 3 March 2016. – access to VEC2TLE software
"Function 'iauPlan94'" (C software source). IAU SOFA C Library. – orbital elements of the major planets

[1] For example, with "VEC2TLE". amsat.org. Archived from the original on 20 May 2016. Retrieved 19 June 2013.

[:0-2] Weber, Bryan. "Orbital Mechanics". Orbital Mechanics. "Orbital Nomenclature", and "Classical Orbital Elements". Retrieved 21 February 2025.{{cite web}}: CS1 maint: url-status (link)

[:02-3] ^ ^a ^b ^c ^d ^e ^f ^g ^h ⁱ ^j Vallado, David A. (2022). Fundamentals of astrodynamics and applications. Space technology library (4th ed.). Torrance, CA: Microcosm Press. pp. 41–112. ISBN 978-1-881883-18-0.

[4] Standish, E. Myles; Williams, James G. "Approximate Positions of the Planets". NASA Solar System Dynamics. Retrieved 20 February 2025.{{cite web}}: CS1 maint: url-status (link)

[Green2-5] Green, Robin M. (1985). Spherical Astronomy. Cambridge University Press. ISBN 978-0-521-23988-2.

[Danby2-6] Danby, J. M. A. (1962). Fundamentals of Celestial Mechanics. Willmann-Bell. ISBN 978-0-943396-20-0.

[Kelso_FAQ2-7] Kelso, T.S. "FAQs: Two-line element set format". celestrak.com. CelesTrak. Archived from the original on 26 March 2016. Retrieved 15 June 2016.

[8] Seidelmann, K.P., ed. (1992). Explanatory Supplement to the Astronomical Almanac (1st ed.). Mill Valley, CA: University Science Books.

[9] "SORCE". Heavens-Above.com. orbit data. Archived from the original on 27 September 2007.

[Aubin-20142-10] Aubin, David (2014). "Delaunay, Charles-Eugène". Biographical Encyclopedia of Astronomers. New York City: Springer New York. pp. 548–549. doi:10.1007/978-1-4419-9917-7_347. ISBN 978-1-4419-9916-0.

[Shevchenko-20172-11] Shevchenko, Ivan (2017). The Lidov–Kozai effect: applications in exoplanet research and dynamical astronomy. Cham: Springer. ISBN 978-3-319-43522-0.

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Common orbital elements by type

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