- $\rho=\Delta\phi$ (N) (conservation of gravitational force)
- $\dot\rho +\nabla\cdot m =0$ (conservation of mass)
- $\dot m +\nabla\cdot (um) +\rho\nabla\phi =0$ (conservation of momentum)
describing a (zero pressure for simplicity) distribution of matter subject to gravitation, where $\rho$ is mass density, $\phi$ gravitational potential, $\nabla\phi$ gravitational force per unit mass, $m$ is momentum, and $u=\frac{m}{\rho}$ is material velocity, all depending on a Euclidean spatial coordinate $x$ plus time $t$ with the dot representing differentiation with respect to time.
We focus on the connection between gravitational potential $\phi$ and mass distribution $\rho$ expressed through Laplace/Poisson's equations (N), which formally involves infinite speed of propagation into $\phi$ from a local change of $\rho$. Let us compare with the following wave equation as a Neo-Newtonian variant of (N) with finite speed of propagation $c$
- $\frac{1}{c^2}\ddot\phi -\Delta\phi = -\rho$. (NN)
Let us now compare (N) and (NN) in a situation where the mass distribution changes/moves with velocity $v$ which is small compared to $c$, which is the typical situation within a planetary system and collection of stars or even galaxy. This means that $\nabla\cdot m$ is small of size $v$, which means that $\dot\rho$ is small of size $v$. We conclude from (NN) that $\dot\phi$ is small of size $v$ and so also $\ddot\phi$ assuming $\nabla\cdot\dot m$ is small of size $v$. This means that the difference between (N) and (NN) is of size $\frac{v}{c^2}$ thus very small.
- For physicists, a strong gravitational wave will produce displacements on the order of $10^{-18}$ meters - this is 1000 times smaller than the diameter of a proton. Waves of this strength will be produced by very massive systems undergoing large accelerations, like two orbiting black holes that are about to merge into one. Since systems like these are rare, these sources will be light-years away. Therefore, the search for gravitational waves is seeking the minute effects of some of the most energetic astrophysical systems from the depths of the universe.
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