Equatorial bulge
An equatorial bulge is a difference between the equatorial and polar diameters of a planet, due to the centrifugal force exerted by the rotation about the body's axis. A rotating body tends to form an oblate spheroid rather than a sphere. The Earth has an equatorial bulge of 42.77 km (26.58 mi); that is, its diameter measured across the equatorial plane (12,756.274 km (7,926.381 mi)) is 42.77 km more than that measured between the poles (12,713.56 km (7,899.84 mi)). An observer standing at sea level on either pole, therefore, is 21.36 km closer to Earth's central point than if standing at sea level on the Equator. The value of Earth's radius may be approximated by the average of these radii.
As a result of Earth's equatorial bulge, the highest point on Earth, measured from the center and outwards, is the peak of Mount Chimborazo in Ecuador rather than Mount Everest. But since the ocean also bulges, like Earth and its atmosphere, Chimborazo is not as high above sea level as Everest is.
The standard formula for this force is the relationship Fc=Mv2/R{displaystyle F_{c}=Mv^{2}/R}
In addition, because Earth's dense core is included in the cross-sectional disc at the Equator, it contributes more to the mass of the disc. Similarly, there is a bulge in the water envelope of the oceans surrounding Earth; this bulge is created by the greater centrifugal force at the Equator and is independent from tides. Sea level at the Equator is 21.36 km higher than that at either pole, in terms of distance from the center of the planet.
Contents
1 The equilibrium as a balance of energies
2 Differences in gravitational acceleration
3 Satellite orbits
4 Other celestial bodies
5 Mathematical expression
6 References
The equilibrium as a balance of energies
Gravity tends to contract a celestial body into a sphere, the shape for which all the mass is as close to the center of gravity as possible. Rotation causes a distortion from this spherical shape; a common measure of the distortion is the flattening (sometimes called ellipticity or oblateness), which can depend on a variety of factors including the size, angular velocity, density, and elasticity.
To get a feel for the type of equilibrium that is involved, imagine someone seated in a spinning swivel chair, with weights in their hands. If the person in the chair pulls the weights towards them, they are doing work and their rotational kinetic energy increases. The increase of rotation rate is so strong that at the faster rotation rate the required centripetal force is larger than with the starting rotation rate.
Something analogous to this occurs in planet formation. Matter first coalesces into a slowly rotating disk-shaped distribution, and collisions and friction convert kinetic energy to heat, which allows the disk to self-gravitate into a very oblate spheroid.
As long as the proto-planet is still too oblate to be in equilibrium, the release of gravitational potential energy on contraction keeps driving the increase in rotational kinetic energy. As the contraction proceeds the rotation rate keeps going up, hence the required force for further contraction keeps going up. There is a point where the increase of rotational kinetic energy on further contraction would be larger than the release of gravitational potential energy. The contraction process can only proceed up to that point, so it halts there.
As long as there is no equilibrium there can be violent convection, and as long as there is violent convection friction can convert kinetic energy to heat, draining rotational kinetic energy from the system. When the equilibrium state has been reached then large scale conversion of kinetic energy to heat ceases. In that sense the equilibrium state is the lowest state of energy that can be reached.
The Earth's rotation rate is still slowing down, though gradually, by about two thousandths of a second per rotation every 100 years.[1] Estimates of how fast the Earth was rotating in the past vary, because it is not known exactly how the moon was formed. Estimates of the Earth's rotation 500 million years ago are around 20 modern hours per "day".
The Earth's rate of rotation is slowing down mainly because of tidal interactions with the Moon and the Sun. Since the solid parts of the Earth are ductile, the Earth's equatorial bulge has been decreasing in step with the decrease in the rate of rotation.
Differences in gravitational acceleration
Red arrow: gravity
Green arrow, the normal force
Blue arrow: the resultant force
The resultant force provides required centripetal force. Without this centripetal force frictionless objects would slide towards the equator.
In calculations, when a coordinate system is used that is co-rotating with the Earth, the vector of the notional centrifugal force points outward, and is just as large as the vector representing the centripetal force.
Because of a planet's rotation around its own axis, the gravitational acceleration is less at the equator than at the poles. In the 17th century, following the invention of the pendulum clock, French scientists found that clocks sent to French Guiana, on the northern coast of South America, ran slower than their exact counterparts in Paris. Measurements of the acceleration due to gravity at the equator must also take into account the planet's rotation. Any object that is stationary with respect to the surface of the Earth is actually following a circular trajectory, circumnavigating the Earth's axis. Pulling an object into such a circular trajectory requires a force. The acceleration that is required to circumnavigate the Earth's axis along the equator at one revolution per sidereal day is 0.0339 m/s². Providing this acceleration decreases the effective gravitational acceleration. At the equator, the effective gravitational acceleration is 9.7805 m/s2. This means that the true gravitational acceleration at the equator must be 9.8144 m/s2 (9.7805 + 0.0339 = 9.8144).
At the poles, the gravitational acceleration is 9.8322 m/s2. The difference of 0.0178 m/s2 between the gravitational acceleration at the poles and the true gravitational acceleration at the equator is because objects located on the equator are about 21 kilometers further away from the center of mass of the Earth than at the poles, which corresponds to a smaller gravitational acceleration.
In summary, there are two contributions to the fact that the effective gravitational acceleration is less strong at the equator than at the poles. About 70 percent of the difference is contributed by the fact that objects circumnavigate the Earth's axis, and about 30 percent is due to the non-spherical shape of the Earth.
The diagram illustrates that on all latitudes the effective gravitational acceleration is decreased by the requirement of providing a centripetal force; the decreasing effect is strongest on the equator.
Satellite orbits
The fact that the Earth's gravitational field slightly deviates from being spherically symmetrical also affects the orbits of satellites through secular orbital precessions.[2][3][4] They depend on the orientation of the Earth's symmetry axis in the inertial space, and, in the general case, affect all the Keplerian orbital elements with the exception of the semimajor axis. If the reference z axis of the coordinate system adopted is aligned along the Earth's symmetry axis, then only the longitude of the ascending node Ω, the argument of pericenter ω and the mean anomaly M undergo secular precessions.[5]
Such perturbations, which were earlier used to map the Earth's gravitational field from space,[6] may play a relevant disturbing role when satellites are used to make tests of general relativity[7] because the much smaller relativistic effects are qualitatively indistinguishable from the oblateness-driven disturbances.
Other celestial bodies
Generally any celestial body that is rotating (and that is sufficiently massive to draw itself into spherical or near spherical shape) will have an equatorial bulge matching its rotation rate. Saturn is the planet with the largest equatorial bulge in Earth's Solar System (11808 km, 7337 miles).
The following is a table of the equatorial bulge of some major celestial bodies of the Solar System:
| Body | Equatorial diameter | Polar diameter | Equatorial bulge | Flattening ratio |
|---|---|---|---|---|
| Earth | 12,756.27 km | 12,713.56 km | 42.77 km | 1:298.2575 |
| Mars | 6,805 km | 6,754.8 km | 50.2 km | 1:135.56 |
| Ceres | 975 km | 909 km | 66 km | 1:14.77 |
| Jupiter | 143,884 km | 133,709 km | 10,175 km | 1:14.14 |
| Saturn | 120,536 km | 108,728 km | 11,808 km | 1:10.21 |
| Uranus | 51,118 km | 49,946 km | 1,172 km | 1:43.62 |
| Neptune | 49,528 km | 48,682 km | 846 km | 1:58.54 |
Equatorial bulges should not be confused with equatorial ridges. Equatorial ridges are a feature of at least three of Saturn's moons: the large moon Iapetus and the tiny moons Atlas, Pan, and Daphnis. These ridges closely follow the moons' equators. The ridges appear to be unique to the Saturnian system, but it is uncertain whether the occurrences are related or a coincidence. The first three were discovered by the Cassini probe in 2005; the Daphnean ridge was discovered in 2017. The ridge on Iapetus is nearly 20 km wide, 13 km high and 1,300 km long. The ridge on Atlas is proportionally even more remarkable given the moon's much smaller size, giving it a disk-like shape. Images of Pan show a structure similar to that of Atlas, while the one on Daphnis is less pronounced.
Mathematical expression
The flattening coefficient f{displaystyle f}
- f=ae−apa=54ω2a3GM=15π41GT2ρ{displaystyle f={frac {a_{e}-a_{p}}{a}}={5 over 4}{omega ^{2}a^{3} over GM}={15pi over 4}{1 over GT^{2}rho }}
where ae=a(1+f3){displaystyle a_{e}=a{bigg (}1+{f over 3}{bigg )}}
a{displaystyle a}
ω=2πT{displaystyle omega ={2pi over T}}
T{displaystyle T}
G{displaystyle G}
M≃43πρa3{displaystyle Msimeq {4 over 3}pi rho a^{3}}
and ρ{displaystyle rho }
References
^ Hadhazy, Adam. "Fact or Fiction: The Days (and Nights) Are Getting Longer". Scientific American. Retrieved 5 December 2011..mw-parser-output cite.citation{font-style:inherit}.mw-parser-output q{quotes:"""""""'""'"}.mw-parser-output code.cs1-code{color:inherit;background:inherit;border:inherit;padding:inherit}.mw-parser-output .cs1-lock-free a{background:url("//upload.wikimedia.org/wikipedia/commons/thumb/6/65/Lock-green.svg/9px-Lock-green.svg.png")no-repeat;background-position:right .1em center}.mw-parser-output .cs1-lock-limited a,.mw-parser-output .cs1-lock-registration a{background:url("//upload.wikimedia.org/wikipedia/commons/thumb/d/d6/Lock-gray-alt-2.svg/9px-Lock-gray-alt-2.svg.png")no-repeat;background-position:right .1em center}.mw-parser-output .cs1-lock-subscription a{background:url("//upload.wikimedia.org/wikipedia/commons/thumb/a/aa/Lock-red-alt-2.svg/9px-Lock-red-alt-2.svg.png")no-repeat;background-position:right .1em center}.mw-parser-output .cs1-subscription,.mw-parser-output .cs1-registration{color:#555}.mw-parser-output .cs1-subscription span,.mw-parser-output .cs1-registration span{border-bottom:1px dotted;cursor:help}.mw-parser-output .cs1-hidden-error{display:none;font-size:100%}.mw-parser-output .cs1-visible-error{font-size:100%}.mw-parser-output .cs1-subscription,.mw-parser-output .cs1-registration,.mw-parser-output .cs1-format{font-size:95%}.mw-parser-output .cs1-kern-left,.mw-parser-output .cs1-kern-wl-left{padding-left:0.2em}.mw-parser-output .cs1-kern-right,.mw-parser-output .cs1-kern-wl-right{padding-right:0.2em}
^ Iorio, L. (2011). "Perturbed stellar motions around the rotating black hole in Sgr A* for a generic orientation of its spin axis". Physical Review D. 84 (12): 124001. arXiv:1107.2916. Bibcode:2011PhRvD..84l4001I. doi:10.1103/PhysRevD.84.124001.
^ Renzetti, G. (2013). "Satellite Orbital Precessions Caused by the Octupolar Mass Moment of a Non-Spherical Body Arbitrarily Oriented in Space". Journal of Astrophysics and Astronomy. 34 (4): 341–348. Bibcode:2013JApA...34..341R. doi:10.1007/s12036-013-9186-4.
^ Renzetti, G. (2014). "Satellite orbital precessions caused by the first odd zonal J3 multipole of a non-spherical body arbitrarily oriented in space". Astrophysics and Space Science. 352 (2): 493–496. Bibcode:2014Ap&SS.352..493R. doi:10.1007/s10509-014-1915-x.
^ King-Hele, D. G. (1961). "The Earth's Gravitational Potential, deduced from the Orbits of Artificial Satellites". Geophysical Journal. 4 (1): 3–16. Bibcode:1961GeoJ....4....3K. doi:10.1111/j.1365-246X.1961.tb06801.x.
^ King-Hele, D. G. (1983). "Geophysical researches with the orbits of the first satellites". Geophysical Journal. 74 (1): 7–23. Bibcode:1983GeoJ...74....7K. doi:10.1111/j.1365-246X.1983.tb01868.x.
^ Renzetti, G. (2012). "Are higher degree even zonals really harmful for the LARES/LAGEOS frame-dragging experiment?". Canadian Journal of Physics. 90 (9): 883–888. Bibcode:2012CaJPh..90..883R. doi:10.1139/p2012-081.
^ "Rotational Flattening". utexas.edu.
