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Large homogeneous gravitating bodies are normally very close to spherical, but if they rotate, they will bulge out at the equator and flatten at the poles, due to centrifugal forces. The flattening parameter is usually given as

where re and rp are the equatorial and polar radii respectively. For uniform density, f can also be expressed as:(a)

where ω is the rotation rate and ρ the uniform density. Most planets have a non-linear decrease in density with radius. For a planet similar to Earth, the effective 'flattening density' is approximately half the average density - the flattening and bulging happen mostly near the surface, where the density is lowest. So we can write

Comparing eqs. (1) and (3) with values(b) for Earth, we get from (1): f =0.0033489 and from (3): f =0.0034493, a difference of 3%. This is due to the assumption that the `flattening density' is approximately half the average density. It is however good enough as a general simplification. To be more accurate, one will have to numerically integrate the density 'shell-by-shell', through the different regions inside Earth and then figure out how to calculate the resultant flattening. Pretty difficult.
Based on the above equations (and stimulated by this month's challenge question), one may perhaps ask the question: how fast must an Earth-like planet spin for it's equatorial gravity to be zero? This is equivalent to the question: at what angular rate will the equatorial centrifugal force cancel out the gravitational force? There are two complicating factors: (i) the equatorial bulge will increase if the planet spins faster than Earth's present rate; (ii) the average density will decrease with increased flattening.
Hence, we are forced back to do numerically integration for small changes in ω until we find a rotation rate and flattening where the equatorial centrifugal force (almost) cancels out the gravitational force, i.e., when
reω2(1+f(e)) = GM/(re rp).(c)
To complicate thing even more, ω and re are dependent variables and eq. (3) includes density, which varies with radius in a non-linear fashion. Hence the requirement for numerical integration. We can use the simplifying approximation that the effective 'flattening density' remains about half the average density of the spheroid, with the average density reducing with the increasing volume.
This gives a critical rotation rate of about 11.25 times Earth's present rotation rate, i.e. a 'day' of about two hours and eight minutes. At the equator, this makes the centrifugal force equal and opposite to the gravitational force (radius about 8,496 km). At the poles (radius about 4,239 km)(d), the gravitational force will be about 10% higher than normal Earth gravity.
The poles may by OK, but one should stay away from the equator of such a planet, because a slight upward movement may make you drift off into space! I also suspect that most of the atmosphere of such a planet may have escaped into space anyway. Not a nice place to be...
-J
(a) Reworked from Wikipedia's 'Equatorial Bulge'.
(b) Earth values: rp = 6,356,752 m, re = 6,378,137 m, ω = 0.0000729115 rad/second and ρavg = 5514.49 kg/m3.
(c) From WGS 84 Ellipsoid (Geoid) chapter III, equation (3-63). The function f(e) is a rather complex eccentricity effect on the gravity at the equator and at the poles. Google "WGS 84 ELLIPSOID 3.1" and download the .pdf if you feel like venturing in there...
(d) It is very interesting that at the 'extreme spin', just before the equatorial surface experiences negative g, the polar radius is about half of the equatorial radius. There may be some deep truth in this, because when black holes spin at the maximum theoretical rate, the polar 'event horizon' is exactly half the equatorial 'event horizon'. The event horizon is called the 'static limit' in rotating (Kerr) black holes. See my post #18 below.
[Last Edited on March 15, 2011 to be in line with WGS 84 Ellipsoid chapter III.)
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