Editing Solar System (section)

=== Scattered disc ===
{{Main|Scattered disc}}

[[File:TheKuiperBelt Projections 100AU Classical SDO.svg|thumb|The orbital eccentricities and inclinations of the scattered disc population compared to the classical and resonant Kuiper belt objects]]
The scattered disc, which overlaps the Kuiper belt but extends out to near 500&nbsp;AU, is thought to be the source of short-period comets. Scattered-disc objects are believed to have been perturbed into erratic orbits by the gravitational influence of [[Formation and evolution of the Solar System#Planetary migration|Neptune's early outward migration]]. Most scattered disc objects have perihelia within the Kuiper belt but aphelia far beyond it (some more than 150&nbsp;AU from the Sun). SDOs' orbits can be inclined up to 46.8° from the ecliptic plane.<ref>{{Cite book |last1=Gomes |first1=R. S. |url=https://www.lpi.usra.edu/books/ssbn2008/7003.pdf |title=The Solar System Beyond Neptune |last2=Fernández |first2=J. A. |last3=Gallardo |first3=T. |last4=Brunini |first4=A. |date=2008 |publisher=University of Arizona Press |isbn=978-0816527557 |pages=259–273 |chapter=The Scattered Disk: Origins, Dynamics, and End States |access-date=12 May 2022 |archive-url=https://web.archive.org/web/20220121172507/https://www.lpi.usra.edu/books/ssbn2008/7003.pdf |archive-date=21 January 2022 |url-status=live}}</ref> Some astronomers consider the scattered disc to be merely another region of the Kuiper belt and describe scattered-disc objects as "scattered Kuiper belt objects".<ref>{{Cite web |last=Jewitt |first=David |date=2005 |title=The 1,000 km Scale KBOs |url=http://www2.ess.ucla.edu/~jewitt/kb/big_kbo.html |url-status=live |archive-url=https://web.archive.org/web/20140609134900/http://www2.ess.ucla.edu/~jewitt/kb/big_kbo.html |archive-date=9 June 2014 |access-date=16 July 2006 |website=University of Hawaii}}</ref> Some astronomers classify centaurs as inward-scattered Kuiper belt objects along with the outward-scattered residents of the scattered disc.<ref>{{Cite web |title=List of Centaurs and Scattered-Disk Objects |url=http://www.minorplanetcenter.org/iau/lists/Centaurs.html |url-status=live |archive-url=https://web.archive.org/web/20170629210646/http://www.minorplanetcenter.org/iau/lists/Centaurs.html |archive-date=29 June 2017 |access-date=2 April 2007 |website=IAU: Minor Planet Center}}</ref>

Currently, there is strong consensus among astronomers that two of the bodies in the scattered disc are {{Visible anchor|Gonggong and Eris|text=dwarf planets}}:
* {{Dp|Eris}} (38.3–97.5&nbsp;AU) is the largest known scattered disc object and the most massive known dwarf planet. Eris's discovery contributed to a debate about the definition of a planet because it is 25% more massive than Pluto<ref name="Brown Schaller 2007">{{Cite journal |last1=Brown |first1=Michael E. |author-link=Michael E. Brown |last2=Schaller |first2=Emily L. |date=15 June 2007 |title=The Mass of Dwarf Planet Eris |journal=Science |volume=316 |issue=5831 |page=1585 |bibcode=2007Sci...316.1585B |doi=10.1126/science.1139415 |pmid=17569855 |s2cid=21468196|url=https://resolver.caltech.edu/CaltechAUTHORS:20121001-135149660 }}</ref> and about the same diameter. It has one known moon, [[Dysnomia (moon)|Dysnomia]]. Like Pluto, its orbit is highly eccentric, with a perihelion of 38.2&nbsp;AU (roughly Pluto's distance from the Sun) and an aphelion of 97.6 AU, and steeply inclined to the ecliptic plane at an angle of 44°.<ref>{{Cite journal |last1=Dumas |first1=C. |last2=Merlin |first2=F. |last3=Barucci |first3=M. A. |last4=de Bergh |first4=C. |last5=Hainault |first5=O. |last6=Guilbert |first6=A. |last7=Vernazza |first7=P. |last8=Doressoundiram |first8=A. |date=August 2007 |title=Surface composition of the largest dwarf planet 136199 Eris (2003 UB{313}) |journal=Astronomy and Astrophysics |volume=471 |issue=1 |pages=331–334 |bibcode=2007A&A...471..331D |doi=10.1051/0004-6361:20066665 |doi-access=free}}</ref>
* {{Dp|Gonggong}} (33.8–101.2&nbsp;AU) is a dwarf planet in a comparable orbit to Eris, except that it is in a 3:10 resonance with Neptune.<ref name="jpldata" group="D">{{Cite web |date=10 April 2017 |title=JPL Small-Body Database Browser: 225088 Gonggong (2007 OR10) |url=https://ssd.jpl.nasa.gov/sbdb.cgi?sstr=2225088 |url-status=live |archive-url=https://web.archive.org/web/20200610013703/https://ssd.jpl.nasa.gov/sbdb.cgi?sstr=2225088 |archive-date=10 June 2020 |access-date=20 February 2020 |publisher=[[Jet Propulsion Laboratory]] |type=20 September 2015 last obs.}}</ref> It has one known moon, [[Xiangliu (moon)|Xiangliu]].<ref name="Kissetal2017">{{Cite journal |last1=Kiss |first1=Csaba |last2=Marton |first2=Gábor |last3=Farkas-Takács |first3=Anikó |last4=Stansberry |first4=John |last5=Müller |first5=Thomas |last6=Vinkó |first6=József |last7=Balog |first7=Zoltán |last8=Ortiz |first8=Jose-Luis |last9=Pál |first9=András |date=16 March 2017 |title=Discovery of a Satellite of the Large Trans-Neptunian Object (225088) 2007 OR<sub>10</sub> |journal=[[The Astrophysical Journal Letters]] |volume=838 |page=5 |arxiv=1703.01407 |bibcode=2017ApJ...838L...1K |doi=10.3847/2041-8213/aa6484 |s2cid=46766640 |id=L1 |doi-access=free |number=1}}</ref>