Editing List of minor-planet groups (section)

== Groups at or beyond the orbit of Neptune ==
* The [[Neptune trojan]]s as of February 2020 consist of 29 objects. The first one to be discovered was {{mpl|2001 QR|322}}.
* [[Trans-Neptunian object]]s (TNOs) are anything with a mean orbital radius greater than 30&nbsp;AU. This classification includes the Kuiper-belt objects (KBOs), the scattered disc, and the Oort cloud.
** [[Kuiper belt|Kuiper-belt]] objects extend from roughly 30&nbsp;AU to 50&nbsp;AU and are broken into the following subcategories:
*** [[Resonant trans-Neptunian object|Resonant objects]] occupy orbital resonances with Neptune, excluding the 1:1 resonance of the Neptune trojans. 
****[[Plutino]]s are by far the most common resonant KBOs and are in a 2:3 resonance with Neptune, just like [[Pluto]]. The perihelion of such an object tends to be close to Neptune's orbit (much as happens with Pluto), but when the object comes to perihelion, Neptune alternates between being 90 degrees ahead of and 90 degrees behind of the object, so there's no chance of a collision. The MPC defines any object with a mean orbital radius between 39&nbsp;AU and 40.5&nbsp;AU to be a plutino. [[90482&nbsp;Orcus]] and [[28978&nbsp;Ixion]] are among the brightest known.
**** Other resonances. There are several known objects in the 1:2 resonance, dubbed ''twotinos'', with a mean orbital radius of 47.7&nbsp;AU and an eccentricity of 0.37. There are several objects in the 2:5 (mean orbital radius of 55&nbsp;AU), 4:7, 4:5, 3:10, 3:5, and 3:4 resonances, among others. The largest in the 2:5 resonance is {{mpl|(84522) 2002 TC|302}}, and the largest in the 3:10 resonance is [[225088 Gonggong]].
*** [[Classical Kuiper belt object|Classical Kuiper-belt objects]], also known as cubewanos (after [[15760 Albion]], which had the provisional designation {{mpl|(15760) 1992 QB|1}} from its 1992 discovery to its 2018 naming), have a mean orbital radius between approximately 40.5&nbsp;AU and 47&nbsp;AU. Cubewanos are objects in the Kuiper belt that didn't get scattered and didn't get locked into a resonance with Neptune. The largest is {{dp|Makemake}}.
** [[Scattered disc]] objects (SDOs) typically have, unlike cubewanos and resonant objects, high-inclination, high-eccentricity orbits with perihelia that are still not too far from Neptune's orbit. They are assumed to be objects that encountered Neptune and were "scattered" out of their originally more circular orbits close to the ecliptic. The most massive known dwarf planet, [[Eris (dwarf planet)|Eris]], belongs to this category.
*** [[Detached object]]s (extended scattered disk) with generally highly elliptical, very large orbits of up to a few hundred AU and a perihelion too far from [[Neptune]]'s orbit for any significant interaction to occur. A more typical member of the extended disk is {{mpl|(148209) 2000 CR|105}}.
****[[Sednoid]]s have perihelia very far removed from the orbit of Neptune. This group is named after the best-known member, [[90377&nbsp;Sedna]]. As of 2020, only 4 objects in this category have been identified, but it is suspected that there are many more.
**The [[Oort cloud]] is a hypothetical cloud of comets with a mean orbital radius between approximately 50,000&nbsp;AU and 100,000&nbsp;AU. No Oort-cloud objects have been detected; the existence of this classification is only inferred from indirect evidence. Some astronomers have tentatively associated [[90377 Sedna|90377&nbsp;Sedna]] with the inner Oort cloud.