Dysnomia (moon): Difference between revisions
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==Properties== |
==Properties== |
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Dysnomia is about 500 times fainter than Eris, and its diameter is estimated to be 100 to 250 km.<ref name="dysnomia"/> The moon is likely too small to be spherical due to self gravity. Combining Keck and Hubble observations, the satellite was used to constrain the mass of Eris, and orbital parameters were estimated. Its orbital period is calculated to be 15.774±0.002 [[day|d]].<ref name=BrownandSchaller2007>{{cite journal | last=Brown |first=M. E. |coauthors=Schaller, E. L. |title=The Mass of Dwarf Planet Eris |journal=Science |volume=316 |issue= |pages=1585 |date=2007 |url= |doi =10.1126/science.1139415 }}</ref> These observations indicate that Dysnomia has a circular orbit around Eris, with a radius of {{nowrap|37 350 ± 140 km.}}<ref name="BrownandSchaller2007"/> This suggests that the mass of Eris is approximately 1.27 times that of Pluto,<ref name="BrownandSchaller2007"/> or approximately 1.65735 x 10^22 kg. |
Dysnomia is about 500 times fainter than Eris, and its diameter is estimated to be 100 to 250 km.<ref name="dysnomia"/> The moon is likely too small to be spherical due to self gravity. Combining Keck and Hubble observations, the satellite was used to constrain the mass of Eris, and orbital parameters were estimated. Its orbital period is calculated to be 15.774±0.002 [[day|d]].<ref name=BrownandSchaller2007>{{cite journal | last=Brown |first=M. E. |coauthors=Schaller, E. L. |title=The Mass of Dwarf Planet Eris |journal=Science |volume=316 |issue= |pages=1585 |date=2007 |url= |doi =10.1126/science.1139415 }}</ref> These observations indicate that Dysnomia has a circular orbit around Eris, with a radius of {{nowrap|37 350 ± 140 km.}}<ref name="BrownandSchaller2007"/> This suggests that the mass of Eris is approximately 1.27 times that of Pluto,<ref name="BrownandSchaller2007"/> or approximately 1.65735 ±0.0889 x 10^22 kg. |
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==Formation== |
==Formation== |
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Revision as of 20:13, 14 April 2010
 Artist's impression of Eris and Dysnomia: Eris is the main object, Dysnomia the smaller disk just above it. The object top-left is the Sun. | |
| Discovery | |
|---|---|
| Discovered by | [note 1] [1] |
| Discovery date | September 10, 2005[1] |
| Designations | |
Designation | (136199) Eris I Dysnomia |
| Pronunciation | /dɪsˈnoʊmiə/; /dаɪsˈnoʊmiə/ [note 2] |
| S/2005 (2003 UB313) 1 | |
| Orbital characteristics [2] | |
| 37 350 ± 140 km | |
| Eccentricity | < 0.013 |
| 15.774 ± 0.002 d | |
| Inclination | 142 ± 3° |
| Satellite of | Eris |
| Physical characteristics | |
Equatorial radius | 50–125 km[3] |
| ~23.1[4] | |
Dysnomia, officially (136199) Eris I Dysnomia, is the only known moon of the dwarf planet Eris (the largest known dwarf planet in the Solar System). It was discovered in 2005 by Mike Brown and the laser guide star adaptive optics team at the W. M. Keck Observatory, and carried the provisional designation of S/2005 (2003 UB313) 1 until officially named Dysnomia[5] (from the Ancient Greek word Δυσνομία meaning "lawlessness") after the daughter of the Greek goddess Eris.
Discovery
During 2005, the adaptive optics team at the Keck telescopes in Hawaii carried out observations of the four brightest Kuiper belt objects (Pluto, Makemake, Haumea, and Eris), using the newly commissioned laser guide star adaptive optics system. Observations taken on 10 September revealed a moon in orbit around Eris, provisionally designated S/2005 (2003 UB313) 1. In keeping with the Xena nickname that was already in use for Eris, the moon was nicknamed "Gabrielle" by its discoverers, after the television warrior princess' sidekick.[6][7]
Properties
Dysnomia is about 500 times fainter than Eris, and its diameter is estimated to be 100 to 250 km.[3] The moon is likely too small to be spherical due to self gravity. Combining Keck and Hubble observations, the satellite was used to constrain the mass of Eris, and orbital parameters were estimated. Its orbital period is calculated to be 15.774±0.002 d.[2] These observations indicate that Dysnomia has a circular orbit around Eris, with a radius of 37 350 ± 140 km.[2] This suggests that the mass of Eris is approximately 1.27 times that of Pluto,[2] or approximately 1.65735 ±0.0889 x 10^22 kg.
Formation
Astronomers now know that three of the four brightest Kuiper belt objects (KBOs) have satellites. Among the fainter members of the belt only about 10% are known to have satellites. This is believed to imply that collisions between large KBOs have been frequent in the past. Impacts between bodies of the order of 1000 km across would throw off large amounts of material which would coalesce into a moon. A similar mechanism is believed to have led to the formation of Earth's own Moon when the Earth was struck by a giant impactor early in the history of the solar system.
Name
Mike Brown, the moon's discoverer, chose the name Dysnomia (Greek: Δυσνομία) due to a number of resonances it possessed for him. Dysnomia, the daughter of Eris, fits the general historically established pattern of naming moons after lesser gods associated with the primary (hence, Jupiter's largest moons are named after lovers of Jupiter, while Saturn's are named after his fellow Titans). Also, the English translation of "Dysnomia", "lawlessness," echoes Lucy Lawless, the actress famous for starring in Xena: Warrior Princess on television. Before receiving their official names, Eris and Dysnomia were known informally as "Xena" and "Gabrielle" respectively (Gabrielle being Xena's sidekick), and Brown decided to retain that honour.
Brown also notes that 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, followed the principle established with Pluto by choosing a name which shared its first four letters with his wife's name, Charlene. "Dysnomia", similarly, has the same first letter as Brown's wife, Diane,[8] and Brown uses the nickname "Dy" /ˈdaɪ/ for the moon, which he pronounces the same as his wife's nickname, Di. Because of this, Brown pronounces the full name /dаɪsˈnoʊmiə/, with a long "y".[9]
In addition, both Eris and Dysnomia, representing aspects of chaos, reflect the effect their existence had in the disputation on the definition of a planet (and specifically on the status of Pluto and Ceres), and the debate that followed.
Notes
- ^ 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, D.L. Rabinowitz, P.J.Stomski Jr., D.M.Summers, C.A.Trujillo, P.L. Wizinowich
- ^ In US dictionary transcription, Template:USdict, or as in Greek Δυσνομία.
References
- ^ a b Michael E. Brown (2006). "Satellites of the largest Kuiper belt objects". Astrophysical Journal Letters. 639 (L43). arXiv:astro-ph/0510029.
{{cite journal}}:|format=requires|url=(help); Unknown parameter|coauthors=ignored (|author=suggested) (help) - ^ a b c d Brown, M. E. (2007). "The Mass of Dwarf Planet Eris". Science. 316 (5831): 1585. doi:10.1126/science.1139415. PMID 17569855.
{{cite journal}}: Unknown parameter|coauthors=ignored (|author=suggested) (help) Cite error: The named reference "BrownandSchaller2007" was defined multiple times with different content (see the help page). - ^ a b Mike Brown. "Dysnomia, the moon of Eris". Caltech. Retrieved 2009-07-02.
- ^ Daniel W. E. Green (2005-10-04). "IAUC 8610: S/2005 (2003 UB_313) 1". International Astronomical Union.
- ^ IAU Circular 8747 - Official publication of the IAU reporting the naming of Eris and Dysnomia (PDF file)
- ^ Deborah Zabarenko (2005-10-03). "Planet Xena has moon called Gabrielle". Australian Broadcasting Corporation. Retrieved 2008-03-09.
- ^ Richard Ingham (2006-02-02). "'Tenth planet' Xena bigger than Pluto". Australian Broadcasting Corporation. Retrieved 2008-03-09.
- ^ Tytell, David (2006-09-14). "All Hail Eris and Dysnomia". Sky & Telescope. Retrieved 2006-12-30.
- ^ "Julia Sweeney and Michael E. Brown". Hammer Conversations: KCET podcast. 2007. Retrieved 2008-06-28. at 42min 12sec
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