Question: [This answer](https://space.stackexchange.com/a/40595/33950) provides quite interesting plots of apogee and perigee for objects 41332 and 41333.

The primary (sine wave -like) oscillations are probably due to perturbations caused by potential generated by non-spherical Earth, as described in [this answer](https://space.stackexchange.com/a/27034/33950) (at least period of few months is in the same order of magnitude with apogee and perigee oscillations for Tiangong-1, as shown in a plot in the [question body](https://space.stackexchange.com/q/26390/33950) to the answer).

But, along with primary oscillation, there are quite strong secondary oscillations of irregular(?) nature shown on the plots:
[![enter image description here](https://i.stack.imgur.com/tWgYR.jpg)](https://i.stack.imgur.com/tWgYR.jpg)

What does look interesting is the symmetry of these otherwise irregular secondary oscillations along vertical line connecting max/min values.

What is/are the reason(s) of these secondary oscillations?

Could it be a measurement noise/error or some weird processing artifacts, or is it indeed the actual behaviour of the orbiting bodies?

Answer: 
Escape from planetary atmospheres of the terrestrial planets in our solar system [is dominated by ions](https://ui.adsabs.harvard.edu/abs/2018A%26A...614L...3G/abstract) in absolute numbers, as opposed to neutral particle species. *Particles* can be any type of molecule or atom here, mostly $\mathrm O^{+}$ and $\mathrm N^{+}$ for Earth. 

For the case of Earth, a particle, once ionised in the upper thermosphere, can couple to the terrestrial magnetic field. From there, it will start orbiting in the magnetosphere, and it can be picked up by the solar wind at the magnetospheric bow-shock. Once transported by the solar wind, most of the species will be transported into interstellar space.

Your argument with the rings of material (not dust, see below) would be valid, if the velocity of the escaping particles would somehow be fine-tuned in a way as to stay in orbit. However, escape velocity from Earth is $14\ \mathrm{km/s}$, the orbital speed at $1\ \mathrm{AU}$ is $30\ \mathrm{km/s}$, so most particles will escape from Earth, not staying in orbit around the sun.  

Add the solar wind on top of that, [having typical speeds of $100{-}400\ \mathrm{km/s}$](https://spaceweather.com/) and you get blown away into space pretty good.

There is of course a small chance that some of those escaped particles will be picked up on their way out by the other planets. This fraction is a function of the geometric cross-section of Hill-sphere of the encountered planets, but is still very small compared to the total escaping flux. I remember having read an article about a fraction of the atoms being lost by Venus, being later picked up by Earth, but can't remember the source.
This results in most gas ending up in interstellar space, as previously stated.

Assuming a constant average velocity of the solar wind of $\sim 100\ \mathrm{km/s}$, the solar wind can traverse the $\sim 150\ \mathrm{AU}$ until interstellar space in just about 6 years. From there, the lost particles contribute to the [interstellar medium](https://en.wikipedia.org/wiki/Interstellar_medium), although in negligible contributions.

Note that a 'dust cloud' is different from escaping atmospheric gas. 'Dust' in space are usually minerals. The most prominent ones are olivines, pyroxenes, forsterites, etc. that form macroscopic crystalline structures and could never escape by Jeans or hydrodynamic escape from an atmosphere, except via meteorite impacts.
Basically it is blown away by the solar wind, headed to interstellar space. A light particle in orbit around the Sun will tend to be pushed further out with time because of both solar wind and photonic pressure. 

Note there are a few pockets of dust around, but they are very hard to see. It takes being in a relatively stable point, usually the L4/ L5 points of a system (Earth-Moon, Earth-Sun) for it to stick around. And that dust is heavier stuff which will stick around easier than a gas.