<p>Encounters between small planetesimals and the larger core of planets (especially Jupiter) transfer momentum between the two. But momentum is conserved. Momentum is:</p>

<p><span class="math-container">$p = m v$</span>, where <span class="math-container">$p$</span> is momentum </p>

<p>So, smaller planetesimals gain more velocity than a larger planet core, for the same momentum exchange. Thus, smaller planetesimals are preferentially boosted to escape the planet, either to be scattered outward to the outer system, or inward to the sun. Some will have the right velocity and aggregate with to core.</p>

<p>Since smaller planetesimals get a larger boost than larger ones, say 1000x rather than 20x (just an example, not real numbers), then they are much more sensitive to initial velocities. Thus a much smaller range of initial velocities will have that exactly right velocity to be captured by the planet, as either a satellite or aggregating with the planet. In the case I just made up, 1000/20 i.e. 50 times narrower. Thus, for an equivalent distribution of velocities, the smaller planetesimals in this example will be 50 times less likely to be captured.</p>

<p>As for dust, beyond it will eventually clump together into larger rocks due to electrostatic attraction, a lot will be sucked into the growing core, or scattered outwards. But it will exert a net drag on the core (see the Grand Tack hypothesis) and gain momentum, and through velocity, energy (a.k.a. heat). And this energy will be averaged out through elastic collisions. Eventually, the dust will either aggregate into larger bodies, sucked into the planet, or scattered into the sun or outwards from the solar system.</p>

CC BY-SA 4.0
2019-02-22T12:52:17.100Z
2019-02-22T13:21:44.050Z
2019-02-22T13:21:44.050Z
Bill Lee
<p>Shouldn't captured moons have the same size distribution as asteroids? And asteroids are more common the smaller size they are. Moons are likely captured if they are in highly inclined orbits, and those moons should've originated as asteroids or Kuiper Belt objects. But there are only <a href="https://en.wikipedia.org/wiki/List_of_natural_satellites#List" rel="noreferrer">two moons</a>, out of 194 known, smaller than 500 meters in radius. Aegaeon and S/2009 S1 both of Saturn. Although it is expected to exist over a million asteroids smaller than that. And all of Pluto's moons were large enough to be found before New Horizons arrived (sorry Alan Stern, no moon for you!)</p>

<ul>
<li><p>Is this purely an observational bias? </p></li>
<li><p>Is it expected that the planets are surrounded by a myriad of moons too small to have been detected yet, from hundreds of meters down to dust grains?</p></li>
<li><p>Do they all somehow gather into planar rings below a certain size? (I think the main line is that a ring system forms as a result of a single collision or tidal crunching event).</p></li>
<li><p>Or what mechanism makes them lack small to tiny moons and dust?</p></li>
</ul>

<p><a href="https://i.sstatic.net/udjxz.png" rel="noreferrer"><img src="https://i.sstatic.net/udjxz.png" alt="https://upload.wikimedia.org/wikipedia/commons/thumb/6/63/Asteroids_by_size_and_number.svg/1024px-Asteroids_by_size_and_number.svg.png"></a></p>

<p><em>How would this asteroid size frequency plot compare to a moon size frequency plot?</em></p>

<asteroids><natural-satellites><size>
Why haven't more captured small moons been found?
LocalFluff
# Why haven't more captured small moons been found?

(Asked by: username_0 on 2018-11-23)

Shouldn't captured moons have the same size distribution as asteroids? And asteroids are more common the smaller size they are. Moons are likely captured if they are in highly inclined orbits, and those moons should've originated as asteroids or Kuiper Belt objects. But there are only [two moons](https://en.wikipedia.org/wiki/List_of_natural_satellites#List), out of 194 known, smaller than 500 meters in radius. Aegaeon and S/2009 S1 both of Saturn. Although it is expected to exist over a million asteroids smaller than that. And all of Pluto's moons were large enough to be found before New Horizons arrived (sorry Alan Stern, no moon for you!)

* Is this purely an observational bias?
* Is it expected that the planets are surrounded by a myriad of moons too small to have been detected yet, from hundreds of meters down to dust grains?
* Do they all somehow gather into planar rings below a certain size? (I think the main line is that a ring system forms as a result of a single collision or tidal crunching event).
* Or what mechanism makes them lack small to tiny moons and dust?

[![https://upload.wikimedia.org/wikipedia/commons/thumb/6/63/Asteroids_by_size_and_number.svg/1024px-Asteroids_by_size_and_number.svg.png](https://i.sstatic.net/udjxz.png)](https://i.sstatic.net/udjxz.png)

*How would this asteroid size frequency plot compare to a moon size frequency plot?*

**Tags:** asteroids, natural-satellites, size


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## 1 answers

### Answer by username_1 on 2019-02-22. Score: 5 | Accepted answer

Encounters between small planetesimals and the larger core of planets (especially Jupiter) transfer momentum between the two. But momentum is conserved. Momentum is:

$p = m v$, where $p$ is momentum

So, smaller planetesimals gain more velocity than a larger planet core, for the same momentum exchange. Thus, smaller planetesimals are preferentially boosted to escape the planet, either to be scattered outward to the outer system, or inward to the sun. Some will have the right velocity and aggregate with to core.

Since smaller planetesimals get a larger boost than larger ones, say 1000x rather than 20x (just an example, not real numbers), then they are much more sensitive to initial velocities. Thus a much smaller range of initial velocities will have that exactly right velocity to be captured by the planet, as either a satellite or aggregating with the planet. In the case I just made up, 1000/20 i.e. 50 times narrower. Thus, for an equivalent distribution of velocities, the smaller planetesimals in this example will be 50 times less likely to be captured.

As for dust, beyond it will eventually clump together into larger rocks due to electrostatic attraction, a lot will be sucked into the growing core, or scattered outwards. But it will exert a net drag on the core (see the Grand Tack hypothesis) and gain momentum, and through velocity, energy (a.k.a. heat). And this energy will be averaged out through elastic collisions. Eventually, the dust will either aggregate into larger bodies, sucked into the planet, or scattered into the sun or outwards from the solar system.


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