In mathematics, a spherical coordinate system is a coordinate system for threedimensional space where the position of a point is specified by three numbers: the radial distance of that point from a fixed origin, its polar angle measured from a fixed zenith direction, and the azimuth angle of its orthogonal projection on a reference plane that passes through the origin and is orthogonal to the zenith, measured from a fixed reference direction on that plane.
The radial distance is also called the radius or radial coordinate. The polar angle may be called colatitude, zenith angle, normal angle, or inclination angle.
The use of symbols and the order of the coordinates differs between sources. In one system frequently encountered in physics (r, θ, φ) gives the radial distance, polar angle, and azimuthal angle, whereas in another system used in many mathematics books (r, θ, φ) gives the radial distance, azimuthal angle, and polar angle. In both systems ρ is often used instead of r. Other conventions are also used, so great care needs to be taken to check which one is being used.
A number of different spherical coordinate systems following other conventions are used outside mathematics. In a geographical coordinate system positions are measured in latitude, longitude and height or altitude. There are a number of different celestial coordinate systems based on different fundamental planes and with different terms for the various coordinates. The spherical coordinate systems used in mathematics normally use radians rather than degrees and measure the azimuthal angle counterclockwise rather than clockwise. The inclination angle is often replaced by the elevation angle measured from the reference plane. Elevation angle of zero is at the horizon.
The concept of spherical coordinates can be extended to higher dimensional spaces and are then referred to as hyperspherical coordinates.
Definition
To define a spherical coordinate system, one must choose two orthogonal directions, the zenith and the azimuth reference, and an origin point in space. These choices determine a reference plane that contains the origin and is perpendicular to the zenith. The spherical coordinates of a point P are then defined as follows:
 The radius or radial distance is the Euclidean distance from the origin O to P.
 The inclination (or polar angle) is the angle between the zenith direction and the line segment OP.
 The azimuth (or azimuthal angle) is the signed angle measured from the azimuth reference direction to the orthogonal projection of the line segment OP on the reference plane.
The sign of the azimuth is determined by choosing what is a positive sense of turning about the zenith. This choice is arbitrary, and is part of the coordinate system's definition.
The elevation angle is 90 degrees (π/2 radians) minus the inclination angle.
If the inclination is zero or 180 degrees (π radians), the azimuth is arbitrary. If the radius is zero, both azimuth and inclination are arbitrary.
In linear algebra, the vector from the origin O to the point P is often called the position vector of P.
Conventions
Several different conventions exist for representing the three coordinates, and for the order in which they should be written. The use of (r, θ, φ) to denote radial distance, inclination (or elevation), and azimuth, respectively, is common practice in physics, and is specified by ISO standard 3111.
However, some authors (including mathematicians) use φ for inclination (or elevation) and θ for azimuth, which "provides a logical extension of the usual polar coordinates notation".^{[1]} Some authors may also list the azimuth before the inclination (or elevation), and/or use ρ instead of r for radial distance. Some combinations of these choices result in a lefthanded coordinate system. The standard convention (r, θ, φ) conflicts with the usual notation for the twodimensional polar coordinates, where θ is often used for the azimuth. It may also conflict with the notation used for threedimensional cylindrical coordinates.
^{[1]}
The angles are typically measured in degrees (°) or radians (rad), where 360° = 2π rad. Degrees are most common in geography, astronomy, and engineering, whereas radians are commonly used in mathematics and theoretical physics. The unit for radial distance is usually determined by the context.
When the system is used for physical threespace, it is customary to use positive sign for azimuth angles that are measured in the counterclockwise sense from the reference direction on the reference plane, as seen from the zenith side of the plane. This convention is used, in particular, for geographical coordinates, where the "zenith" direction is north and positive azimuth (longitude) angles are measured eastwards from some prime meridian.
Major conventions
coordinates 
corresponding local geographical directions $(Z,\backslash \; X,\backslash \; Y)$ 
right/lefthanded

$\backslash \; (r,\backslash \; \backslash theta\_\backslash text\{inc\},\backslash \; \backslash phi\_\backslash text\{az,right\})$ 
$\backslash \; (U,\backslash \; S,\backslash \; E)$ 
right

$\backslash \; (r,\backslash \; \backslash phi\_\backslash text\{az,right\},\backslash \; \backslash theta\_\backslash text\{el\})$ 
$\backslash \; (U,\backslash \; E,\backslash \; N)$ 
right

$\backslash \; (r,\backslash \; \backslash theta\_\backslash text\{el\},\backslash \; \backslash phi\_\backslash text\{az,right\})$ 
$\backslash \; (U,\backslash \; N,\backslash \; E)$ 
left

Note: easting ($E$), northing ($N$), upwardness ($U$). Local azimuth angle would be measured, e.g., counterclockwise from $S$ to $E$ in the case of $(U,\backslash \; S,\backslash \; E)$ .

Unique coordinates
Any spherical coordinate triplet (r, θ, φ) specifies a single point of threedimensional space. On the other hand, every point has infinitely many equivalent spherical coordinates. One can add or subtract any number of full turns to either angular measure without changing the angles themselves, and therefore without changing the point. It is also convenient, in many contexts, to allow negative radial distances, with the convention that (−r, θ, φ) is equivalent to (r, θ + 180°, φ) for any r, θ, and φ. Moreover, (r, −θ, φ) is equivalent to (r, θ, φ + 180°).
If it is necessary to define a unique set of spherical coordinates for each point, one may restrict their ranges. A common choice is:
 r ≥ 0
 0° ≤ θ ≤ 180° (π rad)
 0° ≤ φ < 360° (2π rad)
However, the azimuth φ is often restricted to the interval (−180°, +180°], or (−π, +π] in radians, instead of [0, 360°). This is the standard convention for geographic longitude.
The range [0°, 180°] for inclination is equivalent to [−90°, +90°] for elevation (latitude).
Even with these restrictions, if θ is zero or 180° (elevation is 90° or −90°) then the azimuth angle is arbitrary; and if r is zero, both azimuth and inclination/elevation are arbitrary. To make the coordinates unique, one can use the convention that in these cases the arbitrary coordinates are zero.
Plotting
To plot a point from its spherical coordinates (r, θ, φ), where θ is inclination, move r units from the origin in the zenith direction, rotate by θ about the origin towards the azimuth reference direction, and rotate by φ about the zenith in the proper direction.
Applications
The geographic coordinate system uses the azimuth and elevation of the spherical coordinate system to express locations on Earth, calling them respectively longitude and latitude. Just as the twodimensional Cartesian coordinate system is useful on the plane, a twodimensional spherical coordinate system is useful on the surface of a sphere. In this system, the sphere is taken as a unit sphere, so the radius is unity and can generally be ignored. This simplification can also be very useful when dealing with objects such as rotational matrices.
Spherical coordinates are useful in analyzing systems that have some degree of symmetry about a point, such as volume integrals inside a sphere, the potential energy field surrounding a concentrated mass or charge, or global weather simulation in a planet's atmosphere. A sphere that has the Cartesian equation x^{2} + y^{2} + z^{2} = c^{2} has the simple equation r = c in spherical coordinates.
Two important partial differential equations that arise in many physical problems, Laplace's equation and the Helmholtz equation, allow a separation of variables in spherical coordinates. The angular portions of the solutions to such equations take the form of spherical harmonics.
Another application is ergonomic design, where r is the arm length of a stationary person and the angles describe the direction of the arm as it reaches out.
Three dimensional modeling of loudspeaker output patterns can be used to predict their performance. A number of polar plots are required, taken at a wide selection of frequencies, as the pattern changes greatly with frequency. Polar plots help to show that many loudspeakers tend toward omnidirectionality at lower frequencies.
The spherical coordinate system is also commonly used in 3D game development to rotate the camera around the player's position.
Coordinate system conversions
As the spherical coordinate system is only one of many threedimensional coordinate systems, there exist equations for converting coordinates between the spherical coordinate system and others.
Cartesian coordinates
The spherical coordinates (radius r, inclination θ, azimuth φ) of a point can be obtained from its Cartesian coordinates (x, y, z) by the formulae
 $r=\backslash sqrt\{x^2\; +\; y^2\; +\; z^2\}$
 $\backslash theta\; =\; \backslash operatorname\{arccos\}\backslash left(\backslash frac\{z\}\{r\}\backslash right)$
 $\backslash varphi\; =\; \backslash operatorname\{arctan\}\backslash left(\backslash frac\{y\}\{x\}\backslash right)$
The inverse tangent denoted in φ = arctan(y/x) must be suitably defined, taking into account the correct quadrant of (x,y). See article atan2.
Alternatively, the conversion can be considered as two sequential rectangular to polar conversions: the first in the Cartesian x–y plane from (x,y) to (R,φ), where R is the projection of r onto the x–y plane, and the second in the Cartesian z–R plane from (z,R) to (r,θ). The correct quadrants for φ and θ are implied by the correctness of the planar rectangular to polar conversions.
These formulae assume that the two systems have the same origin, that the spherical reference plane is the Cartesian x–y plane, that θ is inclination from the z direction, and that the azimuth angles are measured from the Cartesian x axis (so that the y axis has φ = +90°). If θ measures elevation from the reference plane instead of inclination from the zenith the arccos above becomes an arcsin, and the cos θ and sin θ below become switched.
Conversely, the Cartesian coordinates may be retrieved from the spherical coordinates (radius r, inclination θ, azimuth φ), where r ∈ Template:Closedopen, φ ∈ Template:Closedclosed, θ ∈ Template:Closedclosed, by:
 $x=r\; \backslash ,\; \backslash sin\backslash theta\; \backslash ,\; \backslash cos\backslash varphi$
 $y=r\; \backslash ,\; \backslash sin\backslash theta\; \backslash ,\; \backslash sin\backslash varphi$
 $z=r\; \backslash ,\; \backslash cos\backslash theta$
Geographic coordinates
To a first approximation, the geographic coordinate system uses elevation angle (latitude) in degrees north of the equator plane, in the range −90° ≤ φ ≤ 90°, instead of inclination. Latitude is either geocentric latitude, measured at the Earth's center and designated variously by ψ, q, φ′, φ_{c}, φ_{g} or geodetic latitude, measured by the observer's local vertical, and commonly designated φ. The azimuth angle (longitude), commonly denoted by λ, is measured in degrees east or west from some conventional reference meridian (most commonly the IERS Reference Meridian), so its domain is −180° ≤ λ ≤ 180°. For positions on the Earth or other solid celestial body, the reference plane is usually taken to be the plane perpendicular to the axis of rotation.
The polar angle, which is 90° minus the latitude and ranges from 0 to 180°, is called colatitude in geography.
Instead of the radial distance, geographers commonly use altitude above some reference surface, which may be the sea level or "mean" surface level for planets without liquid oceans. The radial distance r can be computed from the altitude by adding the mean radius of the planet's reference surface, which is approximately 6,360 ± 11 km for Earth.
However, modern geographical coordinate systems are quite complex, and the positions implied by these simple formulae may be wrong by several kilometers. The precise standard meanings of latitude, longitude and altitude are currently defined by the World Geodetic System (WGS), and take into account the flattening of the Earth at the poles (about 21 km) and many other details.
In astronomy there are a series of spherical coordinate systems that measure the elevation angle from different fundamental planes. These reference planes are the observer's horizon, the celestial equator (defined by the Earth's rotation), the plane of the ecliptic (defined by Earth's orbit around the sun), and the galactic equator (defined by the rotation of the galaxy).
Cylindrical coordinates
Cylindrical coordinates (radius ρ, azimuth φ, elevation z) may be converted into spherical coordinates (radius r, inclination θ, azimuth φ), by the formulas
 $r=\backslash sqrt\{\backslash rho^2\; +\; z^2\}$
 $\backslash theta=\backslash operatorname\{arctan\}(\backslash rho/z)=\backslash operatorname\{arccos\}(z/r)$
 $\backslash varphi=\backslash varphi\; \backslash quad$
Conversely, the spherical coordinates may be converted into cylindrical coordinates by the formulae
 $\backslash rho\; =\; r\; \backslash sin\; \backslash theta\backslash ,$
 $\backslash varphi\; =\; \backslash varphi\backslash ,$
 $z\; =\; r\; \backslash cos\; \backslash theta\backslash ,$
These formulae assume that the two systems have the same origin and same reference plane, measure the azimuth angle φ in the same sense from the same axis, and that the spherical angle θ is inclination from the cylindrical z axis.
Integration and differentiation in spherical coordinates
The following equations assume that θ is inclination from the z (polar) axis (ambiguous since x, y, and z are mutually normal):
The line element for an infinitesimal displacement from $(r,\backslash theta,\backslash varphi)$ to $(r\; +\; \backslash mathrm\{d\}r,\; \backslash ,\backslash theta\; +\; \backslash mathrm\{d\}\backslash theta,\; \backslash ,\; \backslash varphi\; +\; \backslash mathrm\{d\}\backslash varphi)$ is
 $\backslash mathrm\{d\}\backslash mathbf\{r\}\; =\; \backslash mathrm\{d\}r\backslash ,\backslash boldsymbol\{\backslash hat\; r\}\; +\; r\backslash ,\backslash mathrm\{d\}\backslash theta\; \backslash ,\backslash boldsymbol\{\backslash hat\backslash theta\; \}\; +\; r\; \backslash sin\{\backslash theta\}\; \backslash ,\; \backslash mathrm\{d\}\backslash varphi\backslash ,\backslash mathbf\{\backslash boldsymbol\{\backslash hat\; \backslash varphi\}\}.$
where
 $$
\boldsymbol{\hat r}
=\sin (\theta) \cos (\varphi) \boldsymbol{\hat{\imath}} +
\sin (\theta) \sin (\varphi) \boldsymbol{\hat{\jmath}} +
\cos (\theta) \boldsymbol{\hat{k}}
 $\backslash boldsymbol\{\backslash hat\backslash theta\; \}$
=\cos (\theta) \cos (\varphi) \boldsymbol{\hat{\imath}} +
\cos (\theta) \sin (\varphi) \boldsymbol{\hat{\jmath}}
\sin (\theta) \boldsymbol{\hat{k}}
 $$
\boldsymbol{\hat \varphi}
=\sin (\varphi) \boldsymbol{\hat{\imath}} + \cos (\varphi) \boldsymbol{\hat{\jmath}}
are the local orthogonal unit vectors in the directions of increasing $r,\backslash theta,\backslash varphi$, respectively,
and $\backslash boldsymbol\{\backslash hat\{\backslash imath\}\},\; \backslash boldsymbol\{\backslash hat\{\backslash jmath\}\},\; \backslash boldsymbol\{\backslash hat\{k\}\}$ are the unit vectors in cartesian space.
The surface element spanning from $\backslash theta$ to $\backslash theta\; +\; \backslash mathrm\{d\}\backslash theta$ and $\backslash varphi$ to $\backslash varphi\; +\; \backslash mathrm\{d\}\backslash varphi$ on a spherical surface at (constant) radius $r$ is
 $\backslash mathrm\{d\}S\_r=r^2\backslash sin\backslash theta\backslash ,\backslash mathrm\{d\}\backslash theta\backslash ,\backslash mathrm\{d\}\backslash varphi.$
Thus the differential solid angle is
 $\backslash mathrm\{d\}\backslash Omega=\backslash frac\{\backslash mathrm\{d\}S\_r\}\{r^2\}=\backslash sin\backslash theta\backslash ,\backslash mathrm\{d\}\backslash theta\backslash ,\backslash mathrm\{d\}\backslash varphi.$
The surface element in a surface of polar angle $\backslash theta$ constant (a cone with vertex the origin) is
 $\backslash mathrm\{d\}S\_\backslash theta=r\backslash ,\backslash sin\backslash theta\backslash ,\backslash mathrm\{d\}\backslash varphi\backslash ,\backslash mathrm\{d\}r.$
The surface element in a surface of azimuth $\backslash varphi$ constant (a vertical halfplane) is
 $\backslash mathrm\{d\}S\_\backslash varphi=r\backslash ,\backslash mathrm\{d\}r\backslash ,\backslash mathrm\{d\}\backslash theta.$
The volume element spanning from $r$ to $r\; +\; \backslash mathrm\{d\}r$, $\backslash theta$ to $\backslash theta\; +\; \backslash mathrm\{d\}\backslash theta$, and $\backslash varphi$ to $\backslash varphi\; +\; \backslash mathrm\{d\}\backslash varphi$ is
 $\backslash mathrm\{d\}V=r^2\; \backslash sin\; \backslash theta\; \backslash ,\backslash mathrm\{d\}r\backslash ,\backslash mathrm\{d\}\backslash theta\backslash ,\backslash mathrm\{d\}\backslash varphi.$
Thus, for example, a function $f(r,\backslash theta,\backslash varphi)$ can be integrated over every point in R^{3} by the triple integral
 $\backslash int\_\{\backslash varphi=0\}^\{2\; \backslash pi\}\; \backslash int\_\{\backslash theta=0\}^\{\backslash pi\}\; \backslash int\_\{r=0\}^\{\backslash infty\}\; f(r,\backslash theta,\backslash varphi)\; r^2\; \backslash sin\; \backslash theta\; \backslash ,\backslash mathrm\{d\}r\backslash \; \backslash mathrm\{d\}\backslash theta\backslash \; \backslash mathrm\{d\}\backslash varphi.$
The del operator in this system is not defined, and so the gradient, divergence and curl must be defined explicitly:
$\backslash nabla\; f=\{\backslash partial\; f\; \backslash over\; \backslash partial\; r\}\backslash boldsymbol\{\backslash hat\; r\}$
+ {1 \over r}{\partial f \over \partial \theta}\boldsymbol{\hat \theta}
+ {1 \over r\sin\theta}{\partial f \over \partial \varphi}\boldsymbol{\hat \varphi},
$\backslash nabla\backslash cdot\; \backslash mathbf\{A\}\; =\; \backslash frac\{1\}\{r^2\}\{\backslash partial\; \backslash over\; \backslash partial\; r\}\backslash left(\; r^2\; A\_r\; \backslash right)\; +\; \backslash frac\{1\}\{r\; \backslash sin\backslash theta\}\{\backslash partial\; \backslash over\; \backslash partial\backslash theta\}\; \backslash left(\; \backslash sin\backslash theta\; A\_\backslash theta\; \backslash right)\; +\; \backslash frac\{1\}\{r\; \backslash sin\; \backslash theta\}\; \{\backslash partial\; A\_\backslash varphi\; \backslash over\; \backslash partial\; \backslash varphi\},$
$\backslash nabla\; \backslash times\; \backslash mathbf\{A\}\; =\; \backslash displaystyle\{1\; \backslash over\; r\backslash sin\backslash theta\}\backslash left(\{\backslash partial\; \backslash over\; \backslash partial\; \backslash theta\}\; \backslash left(\; A\_\backslash varphi\backslash sin\backslash theta\; \backslash right)$
 {\partial A_\theta \over \partial \varphi}\right) \boldsymbol{\hat r} +
\displaystyle{1 \over r}\left({1 \over \sin\theta}{\partial A_r \over \partial \varphi}
 {\partial \over \partial r} \left( r A_\varphi \right) \right) \boldsymbol{\hat \theta} +
\displaystyle{1 \over r}\left({\partial \over \partial r} \left( r A_\theta \right)
 {\partial A_r \over \partial \theta}\right) \boldsymbol{\hat \varphi},
$\backslash nabla^2\; f=\{1\; \backslash over\; r^2\}\{\backslash partial\; \backslash over\; \backslash partial\; r\}\backslash !\backslash left(r^2\; \{\backslash partial\; f\; \backslash over\; \backslash partial\; r\}\backslash right)$
\! + \!{1 \over r^2\!\sin\theta}{\partial \over \partial \theta}\!\left(\sin\theta {\partial f \over \partial \theta}\right)
\! + \!{1 \over r^2\!\sin^2\theta}{\partial^2 f \over \partial \varphi^2}
= \left(\frac{\partial^2}{\partial r^2} + \frac{2}{r} \frac{\partial}{\partial r}\right)f \! +
{1 \over r^2\!\sin\theta}{\partial \over \partial \theta}\!\left(\sin\theta \frac{\partial}{\partial \theta}\right)f + \frac{1}{r^2\!\sin^2\theta}\frac{\partial^2}{\partial \varphi^2}f.
Kinematics
In spherical coordinates the position of a point is written,
 $\backslash mathbf\{r\}\; =\; r\; \backslash mathbf\{\backslash hat\; r\}$
its velocity is then,
 $\backslash mathbf\{v\}\; =\; \backslash dot\{r\}\; \backslash mathbf\{\backslash hat\; r\}\; +\; r\backslash ,\backslash dot\backslash theta\backslash ,\backslash boldsymbol\{\backslash hat\backslash theta\; \}\; +\; r\backslash ,\backslash dot\backslash varphi\backslash ,\backslash sin\backslash theta\; \backslash mathbf\{\backslash boldsymbol\{\backslash hat\; \backslash varphi\}\}$
and its acceleration is,
 $\backslash mathbf\{a\}\; =\; \backslash left(\; \backslash ddot\{r\}\; \; r\backslash ,\backslash dot\backslash theta^2\; \; r\backslash ,\backslash dot\backslash varphi^2\backslash sin^2\backslash theta\; \backslash right)\backslash mathbf\{\backslash hat\; r\}$
 $+\; \backslash left(\; r\backslash ,\backslash ddot\backslash theta\; +\; 2\backslash dot\{r\}\backslash ,\backslash dot\backslash theta\; \; r\backslash ,\backslash dot\backslash varphi^2\backslash sin\backslash theta\backslash cos\backslash theta\; \backslash right)\; \backslash boldsymbol\{\backslash hat\backslash theta\; \}$
 $+\; \backslash left(\; r\backslash ddot\backslash varphi\backslash ,\backslash sin\backslash theta\; +\; 2\backslash dot\{r\}\backslash ,\backslash dot\backslash varphi\backslash ,\backslash sin\backslash theta\; +\; 2\; r\backslash ,\backslash dot\backslash theta\backslash ,\backslash dot\backslash varphi\backslash ,\backslash cos\backslash theta\; \backslash right)\; \backslash mathbf\{\backslash boldsymbol\{\backslash hat\; \backslash varphi\}\}$
In the case of a constant φ or $\backslash theta=\backslash tfrac\{\backslash pi\}\{2\}$, this reduces to vector calculus in polar coordinates.
See also
Notes
Bibliography
External links
 Template:Springer
 MathWorld description of spherical coordinates
 Coordinate Converter — converts between polar, Cartesian and spherical coordinates
 Spherical Coordinates Animations illustrating spherical coordinates by Frank Wattenberg
 Conventions for Spherical Coordinates Description of the different conventions in use for naming components of spherical coordinates, along with a proposal for standardizing this.


 Two dimensional  

 Three dimensional  


it:Sistema di riferimento#Il sistema sferico
fi:Koordinaatisto#Pallokoordinaatisto
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