Our website is made possible by displaying online advertisements to our visitors.
Please consider supporting us by disabling your ad blocker.
Dysnomia (moon)
&sq=crain_ford&lang=en&file=File:Hubble_Dysnomia_orbit_overlay.jpg) Low-resolution image of Eris and Dysnomia as imaged by the Hubble Space Telescope, August 2006 | |
| Discovery | |
|---|---|
| Discovered by | Brown et al.[a][1] |
| Discovery date | 10 September 2005[1] |
| Designations | |
Designation | Eris I |
| Pronunciation | /dɪsˈnoʊmiə/, /daɪˈsnoʊmiə/[b] |
Named after | Δυσνομία Dysnomia |
| S/2005 (2003 UB313) 1 Dy /ˈdaɪ/ (nickname) Gabrielle (nickname) | |
| Adjectives | Dysnomian |
| Orbital characteristics[2]: 5 | |
| Epoch 31 August 2006 (JD 2453979.0) | |
| 37273±64 km | |
| Eccentricity | 0.0062±0.0010 |
| 15.785899±0.000050 d | |
Average orbital speed | 0.172 km/s[c] |
| Inclination | ≈ 0° (to Eris's equator; assumed) 78.29°±0.65° (to Eris's orbit) 45.49°±0.15° (to celestial equator) 61.59°±0.16° (to ecliptic)[d] |
| 126.17°±0.26° | |
| 180.83°[e] | |
| Satellite of | Eris |
| Physical characteristics | |
| 615+60 −50 km[3]: 7 | |
| Mass | (8.2±5.7)×1019 kg[3]: 6 |
Mean density | 0.7±0.5 g/cm3[3]: 7 |
| synchronous[4] | |
| ≈ 0° to orbit (assumed) | |
| Albedo | 0.05±0.01[3]: 7 |
| 25.4[f] | |
| 5.6[f] | |
Dysnomia (formally (136199) Eris I Dysnomia) is the only known moon of the dwarf planet Eris and is the second-largest known moon of a dwarf planet, after Pluto I Charon. It was discovered in September 2005 by Mike Brown and the Laser Guide Star Adaptive Optics (LGSAO) team at the W. M. Keck Observatory. It carried the provisional designation of S/2005 (2003 UB313) 1 until it was officially named Dysnomia (from the Ancient Greek word Δυσνομία meaning anarchy/lawlessness) in September 2006, after the daughter of the Greek goddess Eris.[6]
With an estimated diameter of 615+60
−50 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.[3]: 8 In stark contrast to Eris's highly-reflective icy surface, Dysnomia has a very dark surface that reflects 5% of incoming visible light,[3] resembling typical trans-Neptunian objects around Dysnomia's size.[7] 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 Orcus, and the Earth–Moon system.
Cite error: There are <ref group=lower-alpha> tags or {{efn}} templates on this page, but the references will not show without a {{reflist|group=lower-alpha}} template or {{notelist}} template (see the help page).
- ^ a b Cite error: The named reference
Brown2006-discoverywas invoked but never defined (see the help page). - ^ a b c Cite error: The named reference
Holler2021was invoked but never defined (see the help page). - ^ a b c d e f Cite error: The named reference
Brown2023was invoked but never defined (see the help page). - ^ Cite error: The named reference
Szakats2022was invoked but never defined (see the help page). - ^ Cite error: The named reference
Grundy-Eriswas invoked but never defined (see the help page). - ^ Cite error: The named reference
IAUC 8747was invoked but never defined (see the help page). - ^ Cite error: The named reference
Brown2018was invoked but never defined (see the help page).
Previous Page Next Page
