13th century illustration of Earth in De sphaera mundi.
Common symbols
${\displaystyle {\mathcal {R}}_{\mathrm {eE} }^{\mathrm {N} }}$, R, ${\displaystyle R_{E}}$
SI unit meter
Other units
mile, kilometer
In SI base units 6.3781×106 m[1]
SI dimension ${\displaystyle [R_{E}]=\mathrm {d} }$ (distance)

Earth radius is the approximate distance from Earth's center to its surface, about 6,371 km (3,959 mi). This distance is used as a unit of length, especially in astronomy and geophysics, where it is usually denoted by R. Strictly speaking, the term "radius" is a property of a true sphere. Since Earth is only approximately spherical, no single value serves as its definitive radius. Meaningful values range from 6,353 to 6,384 kilometres (3,948 to 3,967 mi).

A distance from the center of Earth to some point on its surface might be referred to as Earth’s radius at that point. More commonly, Earth radius means a computed average of distances to the surface or to some idealized surface. The idealized surface is usually mean sea levels globally or else an ellipsoid that approximates sea level.[a] If elevations were to be included, average radius would increase by about 230 m over sea level, or less than one part in 25,000.[2]

The first published reference to the Earth's size appeared around 350 BC, when Aristotle reported in his book On the Heavens[3] that mathematicians had guessed the circumference of the Earth to be 400,000 stadia. Scholars have interpreted Aristotle's figure to be anywhere from highly accurate[4] to almost double the true value.[5] The first known scientific measurement and calculation of the radius of the Earth was performed by Eratosthenes in about 240 BC. Estimates of the accuracy of Eratosthenes’s measurement range from 0.5% to 17%.[6] For both Aristotle and Eratosthenes, uncertainty in the accuracy of their estimates is due to modern uncertainty over which stadion length they meant.

## Introduction

Scale drawing of the oblateness of the 2003 IERS reference ellipsoid. The outer edge of the dark blue line is an ellipse with the same eccentricity as that of the Earth, with north at the top. For comparison, the outer edge of light blue area is a circle of diameter equal to the minor axis. The red line denotes the Karman line and the yellow area, the range of the International Space Station.

Earth's rotation, internal density variations, and external tidal forces cause its shape to deviate systematically from a perfect sphere.[b] Local topography increases the variance, resulting in a surface of profound complexity. Our descriptions of the Earth's surface must be simpler than reality in order to be tractable. Hence, we create models to approximate characteristics of the Earth's surface, generally relying on the simplest model that suits the need.

Each of the models in common use involve some notion of the geometric radius. Strictly speaking, spheres are the only solids to have radii, but broader uses of the term "radius" are common in many fields, including those dealing with models of the Earth. Here is a partial list of models of Earth's surface, ordered from exact to more approximate:

In the case of the geoid and ellipsoids, the fixed distance from any point on the model to the specified center is called "a radius of the Earth" or "the radius of the Earth at that point".[e] It is also common to refer to any mean radius of a spherical model as "the radius of the earth". When considering the Earth's real surface, on the other hand, it is uncommon to refer to a "radius", since there is generally no practical need. Rather, elevation above or below sea level is useful.

Regardless of the model, any radius falls between the polar minimum of about 6,357 km and the equatorial maximum of about 6,378 km (3,950 to 3,963 mi). Hence, the Earth deviates from a perfect sphere by only a third of a percent, which supports the spherical model in many contexts and justifies the term "radius of the Earth". While specific values differ, the concepts in this article generalize to any major planet.

### Physics of Earth's deformation

Rotation of a planet causes it to approximate an oblate ellipsoid/spheroid with a bulge at the equator and flattening at the North and South Poles, so that the equatorial radius a is larger than the polar radius b by approximately aq. The oblateness constant q is given by

${\displaystyle q={\frac {a^{3}\omega ^{2}}{GM}}\,,}$

where ω is the angular frequency, G is the gravitational constant, and M is the mass of the planet.[f] For the Earth 1/q ≈ 289, which is close to the measured inverse flattening 1/f ≈ 298.257. Additionally, the bulge at the equator shows slow variations. The bulge had been decreasing, but since 1998 the bulge has increased, possibly due to redistribution of ocean mass via currents.[8]

The variation in density and crustal thickness causes gravity to vary across the surface and in time, so that the mean sea level differs from the ellipsoid. This difference is the geoid height, positive above or outside the ellipsoid, negative below or inside. The geoid height variation is under 110 m (360 ft) on Earth. The geoid height can change abruptly due to earthquakes (such as the Sumatra-Andaman earthquake) or reduction in ice masses (such as Greenland).[9]

Not all deformations originate within the Earth. The gravity of the Moon and Sun cause the Earth's surface at a given point to undulate by tenths of meters over a nearly 12-hour period (see Earth tide).

Al-Biruni's (973–1048) method for calculation of the Earth's radius improved accuracy.

Given local and transient influences on surface height, the values defined below are based on a "general purpose" model, refined as globally precisely as possible within 5 m (16 ft) of reference ellipsoid height, and to within 100 m (330 ft) of mean sea level (neglecting geoid height).

Additionally, the radius can be estimated from the curvature of the Earth at a point. Like a torus, the curvature at a point will be greatest (tightest) in one direction (north–south on Earth) and smallest (flattest) perpendicularly (east–west). The corresponding radius of curvature depends on the location and direction of measurement from that point. A consequence is that a distance to the true horizon at the equator is slightly shorter in the north/south direction than in the east-west direction.

In summary, local variations in terrain prevent defining a single "precise" radius. One can only adopt an idealized model. Since the estimate by Eratosthenes, many models have been created. Historically, these models were based on regional topography, giving the best reference ellipsoid for the area under survey. As satellite remote sensing and especially the Global Positioning System gained importance, true global models were developed which, while not as accurate for regional work, best approximate the Earth as a whole.

The following radii are fixed and do not include a variable location dependence. They are derived from the World Geodetic System 1984 (WGS-84) standard ellipsoid.[10]

The value for the equatorial radius is defined to the nearest 0.1 m in WGS-84. The value for the polar radius in this section has been rounded to the nearest 0.1 m, which is expected to be adequate for most uses. Refer to the WGS-84 ellipsoid if a more precise value for its polar radius is needed.

The radii in this section are for an idealized surface. Even the idealized radii have an uncertainty of ±2 m.[11] The discrepancy between the ellipsoid radius and the radius to a physical location may be significant. When identifying the position of an observable location, the use of more precise values for WGS-84 radii may not yield a corresponding improvement in accuracy.

The Earth's equatorial radius a, or semi-major axis, is the distance from its center to the equator and equals 6,378.1370 km (3,963.1906 mi).[12] The equatorial radius is often used to compare Earth with other planets.

The Earth's polar radius b, or semi-minor axis, is the distance from its center to the North and South Poles, and equals 6,356.7523 km (3,949.9028 mi).

The distance from the Earth's center to a point on the spheroid surface at geodetic latitude φ is:

${\displaystyle R(\varphi )={\sqrt {\frac {(a^{2}\cos \varphi )^{2}+(b^{2}\sin \varphi )^{2}}{(a\cos \varphi )^{2}+(b\sin \varphi )^{2}}}}}$

where a and b are, respectively, the equatorial radius and the polar radius.

• Maximum: The summit of Chimborazo is 6,384.4 km (3,967.1 mi) from the Earth's center.
• Minimum: The floor of the Arctic Ocean is approximately 6,352.8 km (3,947.4 mi) from the Earth's center.[13]

#### Principal sections

There are two principal radii of curvature: along the meridional and prime-vertical normal sections.

##### Meridional

In particular, the Earth's radius of curvature in the (north–south) meridian at φ is:

${\displaystyle M(\varphi )={\frac {(ab)^{2}}{{\big (}(a\cos \varphi )^{2}+(b\sin \varphi )^{2}{\big )}^{\frac {3}{2}}}}\,.}$

This is the radius that Eratosthenes measured.

##### Prime vertical

If one point had appeared due east of the other, one finds the approximate curvature in the east–west direction.[g]

This radius of curvature in the prime vertical which is perpendicular (normal or orthogonal) to M at geodetic latitude φ is:[h]

${\displaystyle N(\varphi )={\frac {a^{2}}{\sqrt {(a\cos \varphi )^{2}+(b\sin \varphi )^{2}}}}\,.}$

This radius is also called the transverse radius of curvature. At the equator, N = R.

Three different radii as a function of Earth's latitude. R is the geocentric radius; M is the meridional radius of curvature; and N is the prime vertical radius of curvature.

The Earth's meridional radius of curvature at the equator equals the meridian's semi-latus rectum:

b2/a = 6,335.439 km

The Earth's polar radius of curvature is:

a2/b = 6,399.594 km

#### Directional

The Earth's radius of curvature along a course at an azimuth (measured clockwise from north) α at φ is derived from Euler's curvature formula as follows:[14]:97

${\displaystyle R_{\mathrm {c} }={\frac {1}{{\dfrac {\cos ^{2}\alpha }{M}}+{\dfrac {\sin ^{2}\alpha }{N}}}}\,.}$

#### Combinations

It is possible to combine the principal radii of curvature above in a non-directional manner.

The Earth's Gaussian radius of curvature at latitude φ is:[14]

${\displaystyle R_{\mathrm {a} }={\sqrt {MN}}={\frac {a^{2}b}{(a\cos \varphi )^{2}+(b\sin \varphi )^{2}}}\,.}$

The Earth's mean radius of curvature at latitude φ is:[14]:97

${\displaystyle R_{\mathrm {m} }={\frac {2}{{\dfrac {1}{M}}+{\dfrac {1}{N}}}}\,\!}$

The Earth can be modeled as a sphere in many ways. This section describes the common ways. The various radii derived here use the notation and dimensions noted above for the Earth as derived from the WGS-84 ellipsoid;[10] namely,

a = Equatorial radius (6378.1370 km)
b = Polar radius (6356.7523 km)

A sphere being a gross approximation of the spheroid, which itself is an approximation of the geoid, units are given here in kilometers rather than the millimeter resolution appropriate for geodesy.

In geophysics, the International Union of Geodesy and Geophysics (IUGG) defines the mean radius (denoted R1) to be[15]

${\displaystyle R_{1}={\frac {2a+b}{3}}\,\!}$

For Earth, the mean radius is 6,371.0088 km (3,958.7613 mi).[16]

In astronomy, the International Astronomical Union denotes the nominal equatorial Earth radius as ${\displaystyle {\mathcal {R}}_{\mathrm {eE} }^{\mathrm {N} }}$, which is defined to be 6,378.1 km (3,963.2 mi).[1]:3 The nominal polar Earth radius is defined as ${\displaystyle {\mathcal {R}}_{\mathrm {pE} }^{\mathrm {N} }}$ = 6,356.8 km (3,949.9 mi). These values correspond to the zero tide radii. Equatorial radius is conventionally used as the nominal value unless the polar radius is explicitly required.[1]:4

Earth's authalic ("equal area") radius is the radius of a hypothetical perfect sphere that has the same surface area as the reference ellipsoid. The IUGG denotes the authalic radius as R2.[15]

A closed-form solution exists for a spheroid:[17]

${\displaystyle R_{2}={\sqrt {\frac {a^{2}+{\frac {ab^{2}}{\sqrt {a^{2}-b^{2}}}}\ln {\left({\frac {a+{\sqrt {a^{2}-b^{2}}}}{b}}\right)}}{2}}}={\sqrt {{\frac {a^{2}}{2}}+{\frac {b^{2}}{2}}{\frac {\tanh ^{-1}e}{e}}}}={\sqrt {\frac {A}{4\pi }}}\,,}$

where e2 = a2b2/a2 and A is the surface area of the spheroid.

For the Earth, the authalic radius is 6,371.0072 km (3,958.7603 mi).[16]

Another spherical model is defined by the volumetric radius, which is the radius of a sphere of volume equal to the ellipsoid. The IUGG denotes the volumetric radius as R3.[15]

${\displaystyle R_{3}={\sqrt[{3}]{a^{2}b}}\,.}$

For Earth, the volumetric radius equals 6,371.0008 km (3,958.7564 mi).[16]

Another mean radius is the rectifying radius, giving a sphere with circumference equal to the perimeter of the ellipse described by any polar cross section of the ellipsoid. This requires an elliptic integral to find, given the polar and equatorial radii:

${\displaystyle M_{\mathrm {r} }={\frac {2}{\pi }}\int _{0}^{\frac {\pi }{2}}{\sqrt {{a^{2}}\cos ^{2}\varphi +{b^{2}}\sin ^{2}\varphi }}\,d\varphi \,.}$

The rectifying radius is equivalent to the meridional mean, which is defined as the average value of M:[17]

${\displaystyle M_{\mathrm {r} }={\frac {2}{\pi }}\int _{0}^{\frac {\pi }{2}}\!M(\varphi )\,d\varphi \,.}$

For integration limits of [0,π/2], the integrals for rectifying radius and mean radius evaluate to the same result, which, for Earth, amounts to 6,367.4491 km (3,956.5494 mi).

The meridional mean is well approximated by the semicubic mean of the two axes:

${\displaystyle M_{\mathrm {r} }\approx \left({\frac {a^{\frac {3}{2}}+b^{\frac {3}{2}}}{2}}\right)^{\frac {2}{3}}\,,}$

yielding, again, 6,367.4491 km; or less accurately by the quadratic mean of the two axes:

${\displaystyle M_{\mathrm {r} }\approx {\sqrt {\frac {a^{2}+b^{2}}{2}}}\,;}$

about 6,367.454 km; or even just the mean of the two axes:

${\displaystyle M_{\mathrm {r} }\approx {\frac {a+b}{2}}\,;}$

### Average distance from center to surface

Most global mean radii are based on the reference ellipsoid, which approximates the geoid. The geoid has no direct relationship with surface topography, however. An alternative calculation averages elevations everywhere, resulting in a mean radius 230 m larger than the IUGG mean radius, the authalic radius, or the volumetric radius. This average is 6,371.230 km (3,958.899 mi) with uncertainty of 10 m (33 ft).[2]

## Osculating sphere

The best spherical approximation to the ellipsoid in the vicinity of a given point is given by the osculating sphere. Its radius equals the Gaussian radius of curvature as above, the center of the sphere is located at the center of curvature of the ellipsoid, and its radial direction coincides with the ellipsoid normal direction. This concept aids the interpretation of terrestrial and planetary radio occultation refraction measurements.

## Notes

1. ^ See Figure of Earth for a more complete discussion of the models.
2. ^ For details see figure of Earth, geoid, and Earth tide.
3. ^ There is no single center to the geoid; it varies according to local geodetic conditions.
4. ^ In a geocentric ellipsoid, the center of the ellipsoid coincides with some computed center of Earth, and best models the earth as a whole. Geodetic ellipsoids are better suited to regional idiosyncrasies of the geoid. A partial surface of an ellipsoid gets fitted to the region, in which case the center and orientation of the ellipsoid generally do not coincide with the earth's center of mass or axis of rotation.
5. ^ The value of the radius is completely dependent upon the latitude in the case of an ellipsoid model, and nearly so on the geoid.
6. ^ This follows from the International Astronomical Union definition rule (2): a planet assumes a shape due to hydrostatic equilibrium where gravity and centrifugal forces are nearly balanced.[7]
7. ^ East–west directions can be misleading. Point B, which appears due east from A, will be closer to the equator than A. Thus the curvature found this way is smaller than the curvature of a circle of constant latitude, except at the equator. West can be exchanged for east in this discussion.
8. ^ N is defined as the radius of curvature in the plane that is normal to both the surface of the ellipsoid at, and the meridian passing through, the specific point of interest.

## References

1. ^ a b c Mamajek, E. E; Prsa, A; Torres, G; et al. (2015). "IAU 2015 Resolution B3 on Recommended Nominal Conversion Constants for Selected Solar and Planetary Properties". arXiv: [astro-ph.SR].
2. ^ a b Frédéric Chambat; Bernard Valette (2001). "Mean radius, mass, and inertia for reference Earth models" (PDF). Physics of the Earth and Planetary Interiors. 124. pp. 234–253. Retrieved 18 November 2017.
3. ^ Aristotle. On the Heavens. Book II 298 B. Retrieved 5 November 2017.
4. ^ Drummond, William (1817). "On the Science of the Egyptians and Chaldeans, Part I". The Classical Journal. 16: 159.
5. ^
6. ^ "Eratosthenes, the Greek Scientist". Encyclopædia Britannica. 2016.
7. ^
8. ^ Satellites Reveal A Mystery Of Large Change In Earth's Gravity Field , Aug. 1, 2002, Goddard Space Flight Center. Archived April 28, 2010, at the Wayback Machine.
9. ^
10. ^ a b http://earth-info.nga.mil/GandG/publications/tr8350.2/wgs84fin.pdf
11. ^ http://earth-info.nga.mil/GandG/publications/tr8350.2/tr8350.2-a/Chapter%203.pdf
12. ^ "Equatorial Radius of the Earth". Numerical Standards for Fundamental Astronomy: Astronomical Constants : Current Best Estimates (CBEs). IAU Division I Working Group. 2012. Retrieved 2016-08-10.
13. ^ "Discover-TheWorld.com - Guam - POINTS OF INTEREST - Don't Miss - Mariana Trench". Guam.discover-theworld.com. 1960-01-23. Retrieved 2013-09-16.
14. ^ a b c "Geodesy". google.com.br.
15. ^ a b c Moritz, H. (1980). Geodetic Reference System 1980, by resolution of the XVII General Assembly of the IUGG in Canberra.
16. ^ a b c Moritz, H. (March 2000). "Geodetic Reference System 1980". Journal of Geodesy. 74 (1): 128–133. Bibcode:2000JGeod..74..128.. doi:10.1007/s001900050278.
17. ^ a b Snyder, J.P. (1987). Map Projections – A Working Manual (US Geological Survey Professional Paper 1395) p. 16–17. Washington D.C: United States Government Printing Office.