Um, no.
This is a common misconception among people who have a good grasp of classical mechanics (Hi, Physics 107 students!) and a superficial understanding of so-called “modern” physics, i.e. quantum mechanics (QM).
In QM, matter, like electromagnetic forces, is described as both a wave and a particle, leading people to visualize it alternately as one or the other. It’s a conceptual model that is valuable in terms of different mathematical treatments, but doesn’t really convey the true nature of matter as described on the quantum scale. (Skip the next two paragraphs if you don’t want an overly technical explaination of what is going on.)
Particles (electrons, protons, and neutrons) in three-space are described by phi(x,y,z), where phi is, for lack of a better description, a value that describes the amplitude of a probability function for a given energy level, n (which is an integer, at least within an infinite potential well). You therefore can generate a tensor with components of phi that describes the likelyhood of the particle being “at” any given value of x, y, z, and n. The idea that you can actually snapshot the particle and measure its literal position is a false notion, however. You can estimate its position within a radius about a locus x,y,z but only by increasing your uncertainty of the “momentum” of the particle, per the indeterminacy (or uncertainty) principle. There is no actual particle, in the sense of something you can metaphorically hold in your hand; it is better to think of it as a cloud, which is thicker in the middle and wispy on the outside without really having a defined location or boundary.
Each electron, having such a distribution, has limitation on how much their “clouds” can interact. Specifically, electrons are not permitted to be in the same quantum state, per the Pauli Exclusion Principle. That is to say, in relation to any given nucleus, no two electrons can share the same shell, angular momentum (subshell), and spin. They just will not do it, no matter how much you shake them around or how long you wait for them to be at opposite ends of their “orbits”. If you try really, really, really hard, you’ll force the atoms into a degernate state, where electrons have too high a momentum to remain within an orbital, and slide around between nuclei without stopping or attaching themselves to any body, like a cocktail waitress at a dental equipment salesman’s convention. This is called a degenerate state of matter, the post-fusion white dwarf state the Sun will fall into when it has burned up nearly all of the hydrogen and helium. If you push even harder yet (we’re talking supernova-class effort here), then you’ll force the atoms into a state in which electrons will join with protons to make more neutrons (and a bunch of neutrinos, I think…I don’t remember equation balance off-hand) and will compress to a “solid” ball of neutrons or a neutron star. The neutron star is more compact (denser) because the probability distribution of neutrons is much tighter by virtue of being much more massive. Beyond that, you lose any information about the individual particles and collapse into a singularity from which information (matter, light) cannot escape.
The short version is, no, the electrons can’t all just jump to one side and make way for other electrons to just “slip through”, not even given an infinite period. The interaction between the waveforms of two electrons (exclusion principle) in proximity affect each other such that this can’t happen, period, any more than you can miss the ground if gravity just doesn’t notice that you are unsupported. This isn’t to say that you can’t compress the crystilline structure of solid materials (in which there is typically a lot of “unfilled” space) or, given sufficent pressure and time, suffuse one solid material into another, but this requires the atoms to be physically redistributed, not just temporarily “in sync” with each other’s quantum states.
I hope that wasn’t too confusing. Feynman does a better job of explaining this stuff in depth. Try Feynman’s Lectures on Physics, Vol. 3 for a more extensive explaination.
Stranger