As you see, 4D fails to account for the behavior of gravity. At the center of a planet, gravity has to be zero, because gravity is a force and a force has to have a direction, and 4D fails to tell us which direction that force should be. But 4D fails to be taken seriously, not because he is wrong, but because he is not even capable of being merely wrong. His ideas don't connect with the universe that is known and they point at no future experiments to be done.
A little historical excursion into what is known about gravity might shed some light.
Empirically, if a small body, unaffected by air resistance falls near the surface of the earth through 3 equal time periods, in the second time period it falls 3 times as much as in the first, and in the third period it falls 5 times as much as in the first. Galileo established this ratio of 1:3:5 and from it we now say that the distance of a body which starts at rest and falls near the Earth's surface is about -½g(Δt)².
About this time, Kepler was solving the motion of Mars in the sky and determined that the orbits of the planets looked like ellipses and each ellipse had one of it's two focii at the Sun, and that the planets sped up near the sun and got slower away from the sun, such that a line between the sun and a certain planet would sweep out equal areas in equal times, and that the size of the orbits of the planets and the time they needed to go around the Sun was given by a simple power law.
Newton gave us the equations of motion for a body with constant force as s = ½a(Δt)² + v₀Δt +s₀ and v = aΔt + v₀. And Newton defined F = ma. So in the absence of force there is an absence of acceleration, and v is constant.
So from Galileo's experiments, we conclude a = -g (or 9.81 m/s² in the downward direction).
But down in Australia is (famously) not the same direction as down in England. So this "constant" is an illusion caused by the smallness of laboratories compared with the radius of the Earth. And since it is not constant, then it is possible that some observation of how it is not constant will allow one to describe it better.
Newton turned his attention to the heavens, and Kepler's discovery. While constant acceleration gives the simple expressions above, Newton figured out if all the force on a body originates in a straight line from a given point, then a line between that point and the body will sweep out equal areas in equal times. So Kepler's celestial discovery was consistent with Newton's description of Galileo's terrestrial experiments. The fact that Kepler's orbits are ellipses and are fixed in orientation suggested that the acceleration in the direction of the Sun got stronger in inverse proportion to the square of the distance to the sun. And since the simple power-law was found by Kepler, this let Newton demonstrate that exactly one law controlled all the planet's orbits: F ∝ m/r² in the direction of the Sun for all the planets, throughout the solar system.
But Newton knew that in terrestrial experiments forces on bodies in a closed system were balanced. If A put a force on B, then B put an equal and opposite force on A. So it seemed reasonable that the planets which were pulled in the direction of the Sun were being pulled by the Sun and that the Sun was pulled by them an equal amount. naturally a bigger planet would have to pull the sun more to balance out, all other things being equal. So the acceleration of the Sun should be a ∝ ∑ r̂ m/r². But the two forces are part and parcel of the same phenomenon, it would be simpler to write this as F ∝ Mm/r². Adding in a constant of proportionality and the distance, we get F = -r̂ GMm/r² as the theory for the solar system.
But Newton asked himself why must this law only apply to the solar system. What if it were a universal law, and applied to all matter everywhere.
It it were a universal law, then Newton's Shell Theorem showed the gravity of any spherically symmetric object would on the outside look like all the force came from the center of the sphere with the total mass of the sphere. So that the force on the Earth's surface would be "down" and roughly constant. In which case, if the moon were the right distance away, it would describe an ellipse about the Earth with a period of one lunar month. Hurray.
But Newton didn't publish his idea since the astronomer's of his day told him the Moon was at the wrong distance. When they found a mistake and published the new distance, it matched Newton's theory. And so the principle of Universal Gravitation -- that all mass pulls on all mass everywhere came to light of human discovery in the seventeenth century.
It corresponded to what people knew about gravity and the motion of celestial bodies, and it made predictions:
* The moon was the correct distance from the Earth
* High tide happens twice a day, and is a function of the position of the Sun and Moon
* Tiny corrections to Kepler's laws are caused by the pull of planets on each other.
* Comets may move like ellipses, parabolas or hyperbolas
* Planets are necessarily roundish
* It is possible to put a body in orbit about the Earth, etc.
Later, Einstein would close the gap between theory and experiment even more with General Relativity which states in part:
QUOTE
Given a small ball of freely falling test particles initially at rest with respect to each other, the rate at which it begins to shrink is proportional to its volume times: the energy density at the center of the ball, plus the pressure in the x direction at that point, plus the pressure in the y direction, plus the pressure in the z direction.
http://math.ucr.edu/home/baez/einstein/Remarkably, this statement reproduces Newton's Universal gravitation for small masses moving slowly and is better than Newton for fast objects, light and very heavy objects. In the former case it corresponds to reality, and in those latter cases it makes predictions that also turn out to correspond to reality.
a Acceleration of a body, measured in m/s²
F A force upon a body, measured in N = kg m/s²
G Newton's constant, about 0.0000000000667 N m²/kg²
g Standard acceleration of gravity on the Earth's surface, about 9.81 m/s²
M Large central mass, like that of the Sun or Earth, depending on context, measured in kg
m Mass of a body, like an apple, or a planet or the moon, measured in kg
r The distance of an object from the center of a central body, measured in m
r̂ The direction (as a unit vector) of a object from a central body
s Position of a body, measured in m
s₀ Position of a body at time Δt = 0
Δt Elapsed time, measured in s
v Velocity of a body, measured in m/s
v₀ Velocity of a body at time Δt = 0