Content deleted Content added
Lorenzarius (talk | contribs) m zh: |
Add JWST image |
||
| (697 intermediate revisions by more than 100 users not shown) | |||
Line 1:
{{Short description|Moon of Eris}}
{{Other uses|Dysnomia (disambiguation){{!}}Dysnomia}}
{{use dmy dates|date=July 2023}}
{{Infobox planet
| name = Dysnomia
| image = File:Hubble Dysnomia orbit overlay.jpg
| caption = Low-resolution image of [[Eris (dwarf planet)|Eris]] and Dysnomia as imaged by the [[Hubble Space Telescope]], August 2006
| discoverer = [[Michael E. Brown|Brown]] ''et al.''{{efn|name=discoverers|Full list of discoverers are [[Michael E. Brown]], M. A. van Dam, A. H. Bouchez, D. Le Mignant, R. D. Campbell, J. C. Y. Chin, A. Conrad, S. K. Hartman, E. M. Johansson, R. E. Lafon, [[David L. Rabinowitz|D. L. Rabinowitz]], P. J. Stomski Jr., D. M. Summers, [[Chad Trujillo|C. A. Trujillo]], and P. L. Wizinowich.}}<ref name="Brown2006-discovery"/>
| discovered = 10 September 2005<ref name="Brown2006-discovery"/>
| mpc_name = Eris I
| pronounced = {{IPAc-en|d|ɪ|s|ˈ|n|oʊ|m|i|ə}}, {{IPAc-en|d|aɪ|ˈ|s|n|oʊ|m|i|ə}}<ref name="dict-def" group="lower-alpha"/>
| adjectives = Dysnomian
| named_after = [[Dysnomia (deity)|Δυσνομία]] ''Dysnomia''
| alt_names = {{mp|S|2005|2003 UB|313|1}}<br/>Dy {{IPAc-en|ˈ|d|aɪ}} (nickname)<br />Gabrielle (nickname)
| satellite_of = [[Eris (dwarf planet)|Eris]]
| orbit_ref = <ref name="Holler2021"/>{{rp|page=5}}
| apsis = apsis
| epoch = 31 August 2006 ([[Julian day|JD]] 2453979.0)
| semimajor = {{val|37273|64|u=km}}
| eccentricity = {{val|0.0062|0.0010}}
| period = {{val|15.785899|0.000050|ul=d}}
| avg_speed = {{val|0.172|u=km/s}}{{efn|name=avg-speed|The orbital period (P) is {{val|15.774|u=d}}. The orbital circumference (C) is 2π*semi-major axis. Dividing these (P/C) using the correct units gives {{val|0.172|u=km/s}}.}}
| inclination = ≈ {{val|0|ul=°}} {{small|(to Eris's equator; assumed)}}<br/>{{val|78.29|0.65|u=°}} {{small|(to Eris's orbit)}}<br/>{{val|45.49|0.15|u=°}} {{small|(to [[celestial equator]])}}<br/>{{val|61.59|0.16|u=°}} {{small|(to [[ecliptic]])}}{{efn|name=i-ecliptic|Given Dysnomia's orbit pole [[ecliptic latitude]] of +{{val|28.41|0.16|u=°}},<ref name="Holler2021"/>{{rp|page=5}} subtracting this angle from the ecliptic north pole of +90° gives the inclination with respect to the ecliptic: ''i'' {{=}} +90° – (+28.41°) {{=}} +61.59°.}}
| asc_node = {{val|126.17|0.26|u=°}}
| arg_peri = {{val|180.83|u=°}}{{efn|name=arg-peri|Holler et al. (2021) only give the [[longitude of periapsis]] for Dysnomia's orbit, which is {{val|307|12|u=°}}.<ref name="Holler2021"/>{{rp|page=5}} The longitude of periapsis is the sum of the [[ascending node]] and [[argument of periapsis]], so subtracting Dysnomia's ascending node of {{val|126.17|0.26|u=°}} from its longitude of periapsis gives {{val|180.83|u=°}} for its argument of periapsis.}}
| mean_diameter = {{val|615|60|50|u=km}}<ref name="Brown2023"/>{{rp|page=7}}
| mass = {{val|8.2|5.7|e=19|u=kg}}<ref name="Brown2023"/>{{rp|page=6}}
| density = {{val|0.7|0.5|u=g/cm3}}<ref name="Brown2023"/>{{rp|page=7}}
| rotation = [[synchronous rotation|synchronous]]<ref name="Szakats2022"/>
| axial_tilt = ≈ {{val|0|u=°}} {{small|to orbit (assumed)}}
| albedo = {{val|0.05|0.01}}<ref name="Brown2023"/>{{rp|page=7}}
| spectral_type =
| magnitude = 25.4{{efn|name=faint-Eris|Dysnomia's brightness is 1/500 of Eris in the visible band. With ''H'' {{=}} −1.19 for Eris and a magnitude difference of ''Δm'' {{=}} 6.70, this gives ''H'' ≈ 5.6 for Dysnomia.<ref name="Grundy-Eris"/>}}
| abs_magnitude = 5.6{{efn|name=faint-Eris}}
}}
'''Dysnomia''', formal designation '''(136199) Eris I''', is the only known [[natural satellite|moon]] of the [[dwarf planet]] [[Eris (dwarf planet)|Eris]] and is the second-largest known moon of a dwarf planet, after [[Charon (moon)|Pluto I Charon]]. It was discovered in September 2005 by [[Michael E. Brown|Mike Brown]] and the Laser Guide Star [[Adaptive Optics]] (LGSAO) team at the [[W. M. Keck Observatory]]. It carried the [[provisional designation]] of '''{{mp|S|2005|2003 UB|313|1}}''' until it was officially named ''Dysnomia'' (from the Ancient Greek word {{lang|grc|Δυσνομία}} meaning anarchy/lawlessness) in September 2006, after the [[Dysnomia (deity)|daughter]] of the Greek goddess [[Eris (mythology)|Eris]].<ref name="IAUC 8747"/>
With an estimated diameter of {{val|615|60|50|u=km}}, Dysnomia spans 24% to 29% of Eris's diameter. It is significantly less massive than Eris, with a density consistent with it being mainly composed of ice.<ref name="Brown2023"/>{{rp|page=8}} In stark contrast to Eris's highly-reflective icy surface, Dysnomia has a very dark surface that reflects 5% of incoming visible light,<ref name="Brown2023"/> resembling typical [[trans-Neptunian object]]s around Dysnomia's size.<ref name="Brown2018"/> These physical properties indicate Dysnomia likely formed from a large impact on Eris, in a similar manner to other binary dwarf planet systems like Pluto and {{dp|Orcus}}, and the Earth–Moon system.
==
In 2005, the [[adaptive optics]] team at the [[Keck telescopes]] in [[Hawaii]] carried out observations of the four brightest [[Kuiper belt]] objects ([[Pluto]], {{dp|Makemake}}, {{dp|Haumea}}, and {{dp|Eris}}), using the newly commissioned [[laser guide star]] adaptive optics system. Observations taken on 10 September 2005, revealed a [[natural satellite|moon]] in orbit around Eris, provisionally designated {{mp|S|2005|2003 UB|313|1}}. In keeping with the ''[[Xena]]'' nickname that was already in use for Eris, the moon was nicknamed "[[Gabrielle (Xena: Warrior Princess)|Gabrielle]]" by its discoverers, after Xena's sidekick.<ref name="ABC-Zabarenko"/><ref name="ABC-Ingham"/>
== Physical characteristics ==
[[File:ESO-L. Calçada - Eso1142c (by).jpg|thumb|left|alt=Dysnomia|Artist's conception of Dysnomia's dark surface, with dwarf planet Eris in the background]]
[[File:Eris and moon Dysnomia JWST NIRCam.jpg|thumb|left|Eris and Dysnomia (lower left) imaged by the [[James Webb Space Telescope]] [[NIRCam]] in August 2024]]
[[Submillimeter]]-wavelength observations of the Eris–Dysnomia system's [[thermal radiation|thermal emission]]s by the [[Atacama Large Millimeter Array]] (ALMA) in 2015<!--clarify--> first showed that Dysnomia had a large diameter and a very low albedo, with the initial estimate being {{val|700|115|u=km}}.<ref name="Brown2018"/> Further observations by ALMA in 2018<!--clarify--> refined Dysnomia's diameter to {{val|615|60|50|u=km}} (24% to 29% of Eris's diameter) and an [[albedo]] of {{val|0.05|0.01}}.<ref name="Brown2023"/> Of the known moons of dwarf planets, only [[Charon (moon)|Charon]] is larger, making Dysnomia the second-largest moon of a dwarf planet.<ref name="Lakdawalla2018">{{cite web|title=Some big moons in the Kuiper belt|url=https://www.planetary.org/blogs/emily-lakdawalla/2018/0202-big-moons-dysnomia-vanth.html|first=Emily|last=Lakdawalla|publisher=The Planetary Society|date=25 January 2018}}</ref> Dysnomia's low albedo significantly contrasts with Eris's extremely high albedo of 0.96; its surface has been described to be darker than [[coal]],<ref name="Lakdawalla2018"/> which is a typical characteristic seen in trans-Neptunian objects around Dysnomia's size.<ref name="Brown2018"/>
Eris and Dysnomia are mutually [[tidally locked]], like Pluto and Charon. [[Astrometry|Astrometric]] observations of the Eris–Dysnomia system by ALMA show that Dysnomia does not induce detectable [[barycenter|barycentric]] wobbling in Eris's position, implying its mass must be less than {{val|1.4|e=20|u=kg}} (mass ratio {{val|0.0050|0.0035}}).<ref name="Brown2023"/> This is below the estimated mass range of {{val|2|-|5|e=20|u=kg}} (mass ratio 0.01–0.03) that would normally allow Eris to be tidally locked within the range of the Solar System,<ref name=Szakats2022/> suggesting that Eris must therefore be unusually dissipative.<ref name=Brown2023/> ALMA's upper-limit mass estimate for Dysnomia corresponds to an upper-limit density of {{val|1.2|u=g/cm3|p=< }}, implying a mostly icy composition.<ref name="Brown2023"/> The shape of Dysnomia is not known, but its low density suggests that it should not be in hydrostatic equilibrium.<ref name="Grundy2019">{{cite journal
|first1=W. M. |last1=Grundy
|first2=K. S. |last2=Noll
|first3=M. W. |last3=Buie
|first4=S. D. |last4=Benecchi
|first5=D. |last5=Ragozzine
|first6=H. G. |last6=Roe
|title=The Mutual Orbit, Mass, and Density of Transneptunian Binary Gǃkúnǁʼhòmdímà ({{mp|(229762) 2007 UK|126}})
|url=http://www2.lowell.edu/~grundy/abstracts/2019.G-G.html
|journal=Icarus
|doi=10.1016/j.icarus.2018.12.037
|date=December 2018
|volume=334
|page=30
|bibcode=2019Icar..334...30G
|s2cid=126574999
|archive-url=https://web.archive.org/web/20190407045339/http://www2.lowell.edu/~grundy/abstracts/preprints/2019.G-G.pdf
|archive-date=7 April 2019|url-access=subscription
}}</ref>
The brightness difference between Dysnomia and Eris decreases with longer and redder wavelengths; Hubble Space Telescope observations show that Dysnomia is 500 times fainter than Eris (6.70-magnitude difference) in visible light,<ref name="Dysnomia"/><ref name="Grundy-Eris"/> whereas [[near-infrared]] Keck telescope observations show that Dysnomia is ~60 times fainter (4.43-magnitude difference) than Eris.<ref name="IAUC 8610"/> This indicates Dysnomia has a very different spectrum and redder color than Eris, indicating a significantly darker surface, something that has been proven by submillimeter observations.<ref name="Sicardy Ortiz et al. 2011"/><ref name="Brown2018"/>
== Orbit ==
[[File:Binary dwarf planets scale comparison.png|thumb|upright=2|Diagram of three binary trans-Neptunian dwarf planets and their satellites with true colors, diameters, and distances to scale. Each system's barycenter position marked is in red crosshairs.]]
Combining Keck and Hubble observations, the orbit of Dysnomia was used to determine the mass of Eris through [[Kepler's laws of planetary motion#Third law|Kepler's third law of planetary motion]]. Dysnomia's average orbital distance from Eris is approximately {{cvt|37300|km|mi}}, with a calculated orbital period of 15.786 days, or approximately half a month.<ref name="Holler2021"/> This shows that the mass of Eris is 1.27 times that of Pluto.<ref name="Brown Schaller 2007"/><ref name="Brown2007sup"/> Extensive observations by Hubble indicate that Dysnomia has a nearly circular orbit around Eris, with a low [[orbital eccentricity]] of {{val|0.0062|0.0010}}. Over the course of Dysnomia's orbit, its distance from Eris varies by {{cvt|462 ± 105|km|mi}} due to its slightly eccentric orbit.<ref name="Holler2021"/>
Dynamical simulations of Dysnomia suggest that its orbit should have completely [[Tidal circularization|circularized]] through mutual tidal interactions with Eris within timescales of 5–17 million years, regardless of the moon's density. A non-zero eccentricity would thus mean that Dysnomia's orbit is being perturbed, possibly due to the presence of an additional inner satellite of Eris. However, it is possible that the measured eccentricity is not real, but due to interference of the measurements by albedo features, or systematic errors.<ref name="Holler2021"/>
From Hubble observations from 2005 to 2018, the inclination of Dysnomia's orbit with respect to Eris's [[heliocentric]] orbit is calculated to be approximately 78°. Since the inclination is less than 90°, Dysnomia's orbit is therefore [[prograde and retrograde motion|prograde]] relative to Eris's orbit. In 2239, Eris and Dysnomia will enter a period of mutual events in which Dysnomia's orbital plane is aligned edge-on to the Sun, allowing for Eris and Dysnomia to take turns [[eclipse|eclipsing]] each other.<ref name="Holler2021"/>
== Formation ==
Eight of the ten largest trans-Neptunian objects are known to have at least one satellite. Among the fainter members of the trans-Neptunian population, only about 10% are known to have satellites.<ref name="Brown2023"/> This is thought to imply that collisions between large KBOs have been frequent in the past. Impacts between bodies of the order of {{val|1000|u=km}} across would throw off large amounts of material that would coalesce into a moon. A similar mechanism is thought to have led to the formation of the [[Moon]] when [[Earth]] was [[impact event|struck]] by [[Theia (planet)|a giant impactor]] (see [[Giant impact hypothesis]]) early in the history of the [[Solar System]].<ref name="Brown2023"/>
== Name ==
Mike Brown, the moon's discoverer, chose the name ''Dysnomia'' for the moon. As the daughter of Eris, the mythological [[Dysnomia (deity)|Dysnomia]] fit the established pattern of naming moons after gods associated with the primary body (hence, [[Jupiter]]'s largest moons are named after lovers of [[Jupiter (mythology)|Jupiter]], while [[Saturn]]'s are named after his fellow Titans). The English translation of Dysnomia, "lawlessness", also echoes [[Lucy Lawless]], the actress who played Xena in ''[[Xena: Warrior Princess]]'' on television. Before receiving their official names, Eris and Dysnomia had been nicknamed "Xena" and "Gabrielle", though Brown states that the connection was accidental.<ref>{{Cite book |last=Brown |first=Mike |author-link=Michael E. Brown |title=How I Killed Pluto and Why It Had It Coming |title-link=How I Killed Pluto and Why It Had It Coming |date=2012 |publisher=[[Random House]] |isbn=978-0-385-53110-8 |___location=New York |page=239}}</ref>
A primary reason for the name was its similarity to the name of Brown's wife, Diane, following a pattern established with Pluto. Pluto owes its name in part to its first two letters, which form the initials of [[Percival Lowell]], the founder of the observatory where its discoverer, [[Clyde Tombaugh]], was working, and the person who inspired the search for "[[Planet X]]". [[James Christy]], who discovered [[Charon (moon)|Charon]], did something similar by adding the Greek ending ''-on'' to ''Char'', the nickname of his wife Charlene. (Christy wasn't aware that the resulting 'Charon' was a figure in Greek mythology.) "Dysnomia", similarly, has the same first letter as Brown's wife, Diane.<ref name="SkyTel"/>
== Notes ==
{{notelist|refs=
<ref name="dict-def">
Brown uses the latter pronunciation at [https://www.youtube.com/watch?v=7pbj_llmiMg How I Killed Pluto and Why It Had It Coming]{{rp|at=56:00, 1:06:17|style=ama}}
</ref>
}}
== References ==
{{reflist
|refs =
<ref name="Brown2006-discovery">
{{cite journal
|last1=Brown |first1=M. E.
|date=2006
|title=Satellites of the Largest Kuiper Belt Objects
|url=http://web.gps.caltech.edu/~mbrown/papers/ps/gab.pdf
|journal=[[Astrophysical Journal Letters]]
|volume=639 |issue=1 |pages=L43–L46
|arxiv=astro-ph/0510029
|bibcode=2006ApJ...639L..43B
|doi=10.1086/501524
|s2cid=2578831
|access-date=2011-10-19
|display-authors=etal}}</ref>
<ref name="Brown Schaller 2007">
{{cite journal
|last1=Brown |first1=M. E.
|last2=Schaller |first2=E. L.
|date=2007
|title=The Mass of Dwarf Planet Eris
|journal=[[Science (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>
<ref name="Brown2007sup">
{{cite journal
|url=https://www.science.org/doi/10.1126/science.1139415
|last1=Brown |first1=M. E.
|last2=Schaller |first2=E. L.
|date=2007
|title=Supporting Online Material for The Mass of Dwarf Planet Eris
|journal=Science |volume=316 |issue=5831 |pages=1585 |doi=10.1126/science.1139415 |pmid=17569855 |bibcode=2007Sci...316.1585B |s2cid=21468196 |access-date=2 February 2019
|url-access=subscription }}</ref>
<!-- Not in use
<ref name="johnston">
{{cite web
|last=Johnston |first=W. R.
|date=30 December 2008
|title=(136199) Eris and Dysnomia
|url=http://www.johnstonsarchive.net/astro/astmoons/am-136199.html
|work=Johnston's Archive
|access-date=2012-04-12
}}</ref>
<ref name=TNOCool4>
{{cite journal
|last=Santos-Sanz |first=P.
|date=2012
|title="TNOs are Cool": A Survey of the Transneptunian Region IV. Size/albedo characterization of 15 scattered disk and detached objects observed with Herschel Space Observatory-PACS
|arxiv=1202.1481
|display-authors=etal
|doi=10.1051/0004-6361/201118541
|volume=541
|journal=Astronomy & Astrophysics
|page=A92
|bibcode=2012A&A...541A..92S|s2cid=118600525
}}</ref>
Not in use-->
<ref name="Dysnomia">
{{cite web
|last=Brown |first=M. E.
|date=14 June 2007
|title=Dysnomia, the moon of Eris
|url=http://www.gps.caltech.edu/~mbrown/planetlila/moon
|publisher=[[Caltech]]
|access-date=2011-07-03
}}</ref>
<ref name="IAUC 8610">
{{cite journal
|last=Green |first=D. W. E.
|date=4 October 2005
|title=S/2005 ({{mp|2003 UB|313}}) 1
|url=http://www.cbat.eps.harvard.edu/iauc/08600/08610.html
|journal=[[IAU Circular]]
|issue=8610
|access-date=12 January 2012
|ref={{sfnRef|IAUC 8610}}
}}</ref>
<ref name="IAUC 8747">
{{cite journal
|last=Green |first=D. W. E.
|title=(134340) Pluto, (136199) Eris, and (136199) Eris I (Dysnomia)
|date=13 September 2006
|journal=[[IAU Circular]]
|issue=8747
|page=1
|bibcode=2006IAUC.8747....1G
|url=http://www.cbat.eps.harvard.edu/iauc/08700/08747.html
|access-date=12 January 2012
|ref={{sfnRef|IAUC 8747}}
}}</ref>
<ref name="ABC-Zabarenko">
{{cite news
|last=Zabarenko |first=D.
|date=3 October 2005
|title=Planet Xena has moon called Gabrielle
|url=http://www.abc.net.au/science/news/stories/s1473136.htm
|work=[[Australian Broadcasting Corporation]]
|access-date=9 March 2008
}}</ref>
<ref name="ABC-Ingham">
{{cite news
|last=Ingham |first=R.
|date=2 February 2006
|title='Tenth planet' Xena bigger than Pluto
|work=[[Australian Broadcasting Corporation]]
|url=http://www.abc.net.au/science/news/stories/s1560563.htm
|access-date=9 March 2008
}}
</ref>
<ref name="Sicardy Ortiz et al. 2011">
{{cite journal
|last1=Sicardy |first1=B.
|date=2011
|title=A Pluto-like radius and a high albedo for the dwarf planet Eris from an occultation
|url=http://hal.upmc.fr/docs/00/63/77/20/PDF/Eris_SI.pdf
|journal=[[Nature (journal)|Nature]]
|volume=478 |issue=7370 |pages=493–496
|bibcode= 2011Natur.478..493S
|doi=10.1038/nature10550
|pmid=22031441
|hdl=11336/36807
|s2cid=4422527
|ref={{sfnRef|Sicardy Ortiz et al.|2011}}
|display-authors=etal}}</ref>
<ref name="SkyTel">{{cite news
|last=Tytell
|first=D.
|date=14 September 2006
|title=All Hail Eris and Dysnomia
|work=[[Sky & Telescope]]
|url=http://skytonight.com/news/home/3916126.html
|access-date=30 December 2006
|archive-date=19 October 2006
|archive-url=https://web.archive.org/web/20061019195725/http://skytonight.com/news/home/3916126.html
|url-status=dead
}}</ref>
<!-- unused <ref name="pluggdTV-Hammer">
{{cite web
|date=2007
|title=Julia Sweeney and Michael E. Brown
|work=Hammer Conversations: KCET podcast
|url=http://www.pluggd.tv/audio/channels/kcet_podcast__hammer_conversations/episodes/2h10l
|access-date=28 June 2008
|at=42 min 12 sec
|archive-url=https://web.archive.org/web/20080626220548/http://www.pluggd.tv/audio/channels/kcet_podcast__hammer_conversations/episodes/2h10l
|archive-date=26 June 2008
}}</ref> -->
<ref name="Brown2018">{{cite journal
|first1 = Michael E. |last1 = Brown
|first2 = Bryan J. |last2 = Butler
|title = Medium-sized satellites of large Kuiper belt objects
|journal = The Astronomical Journal
|date = October 2018
|volume = 156
|issue = 4
|pages = 6
|id = 164
|doi-access = free
|doi = 10.3847/1538-3881/aad9f2
|arxiv = 1801.07221
|bibcode = 2018AJ....156..164B
|s2cid = 119343798}}</ref>
<ref name="Holler2021">
{{cite journal
|last1=Holler |first1=Bryan J.
|last2=Grundy |first2=William M.
|last3=Buie|first3=Marc W.
|last4=Noll |first4=Keith S.
|title=The Eris/Dysnomia system I: The orbit of Dysnomia
|journal=Icarus
|date=February 2021
|volume=355
|article-number=114130
|id=114130
|doi=10.1016/j.icarus.2020.114130
|arxiv=2009.13733
|bibcode=2021Icar..35514130H
|s2cid=221995416
}}</ref>
<ref name="Szakats2022">{{cite journal
|display-authors = etal
|first1 = R. |last1 = Szakáts
|first2 = Cs. |last2 = Kiss
|first3 = J. L. |last3 = Ortiz
|first4 = N. |last4 = Morales
|first5 = A. |last5 = Pál
|first6 = T. G. |last6 = Müller
|title = Tidally locked rotation of the dwarf planet (136199) Eris discovered from long-term ground based and space photometry
|journal = Astronomy & Astrophysics
|date = November 2022
|volume = 669 |doi = 10.1051/0004-6361/202245234 |arxiv = 2211.07987
|bibcode = 2023A&A...669L...3S |s2cid = 253522934 }}</ref>
<ref name="Brown2023">{{cite journal |last1=Brown |first1=Michael E. |last2=Butler |first2=Bryan J. |title=Masses and Densities of Dwarf Planet Satellites Measured with ALMA |journal=The Planetary Science Journal |date=1 October 2023 |volume=4 |issue=10 |pages=193 |doi=10.3847/PSJ/ace52a|doi-access=free |arxiv=2307.04848 |bibcode=2023PSJ.....4..193B }}</ref>
<ref name="Grundy-Eris">{{cite web
|title = Eris and Dysnomia (136199 2003 UB313)
|url = http://www2.lowell.edu/users/grundy/tnbs/136199_2003_UB313_Eris.html
|first = Will |last = Grundy
|website = Lowell Observatory
|date = 21 March 2022
|access-date = 16 November 2022}}</ref>
}}
==External links==
* {{Commons category-inline|Dysnomia}}
{{Eris}}
{{Solar System moons (compact)}}
{{Moons of dwarf planets}}
{{Solar System}}
{{Portal bar|Astronomy|Stars|Spaceflight|Outer space|Solar system}}
{{DEFAULTSORT:Dysnomia (Moon)}}
[[Category:Moons of dwarf planets]]
[[Category:Eris (dwarf planet)]]
[[Category:Discoveries by Michael E. Brown]]
[[Category:Astronomical objects discovered in 2005|20050910]]
[[Category:Discoveries by Chad Trujillo]]
[[Category:Discoveries by David L. Rabinowitz]]
[[Category:Solar System]]
| |||