Dysnomia (satelit) Note | Meniu de navigaretext„Satellites of the Largest Kuiper Belt...
ErisObiecte astronomice descoperite în 2005Sateliți naturali
greacăsatelitErisobiect trans-neptuniancentura lui KuiperMichael E. BrownDysnomiaEris
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Dysnomia (satelit)
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| Dysnomia | |
 Dysnomia, la stânga și Eris în centru (Telescopul spațial Hubble) | |
| Denumiri alternative | (136199) Eris I Dysnomia |
|---|---|
| Numit după | Dysnomia |
| Date generale | |
| Descoperire | Mike Brown 10 septembrie 2005[1] |
| Caracteristicile orbitei | |
| Semiaxa mare | 37.350 ± 140 km[2] |
| Excentricitatea | < 0,013 |
| Perioada siderală | 15,774 ± 0,002 zile |
| Înclinarea față de ecliptică | 142 ± 3° |
| Date fizice | |
| Magnitudine absolută | ~3,2[3][4] |
| Magnitudine aparentă | ~23,1[4] |
Modifică text  | |
Dysnomia, denumire oficială (136199) Eris I Dysnomia (greacă: Δυσνομία), este singurul satelit cunoscut al planetei Eris, care este un obiect trans-neptunian din centura lui Kuiper. A fost descoperit la 10 septembrie 2005 de către Michael E. Brown și a fost denumit provizoriu S/2005 (2003 UB313) 1. Numele de Dysnomia provine din cuvântul grec Δυσνομία având sensul de fărădelege. Satelitul a fost denumit după Dysnomia - fiica zeiței discordiei, Eris.
Note |
^
Brown, M. E. (2006). „Satellites of the Largest Kuiper Belt Objects” (PDF). Astrophysical Journal Letters. 639 (1): L43. arXiv:astro-ph/0510029
. Bibcode:2006ApJ...639L..43B. doi:10.1086/501524. Accesat în 19 octombrie 2011. Citare cu parametru depășit |coauthors=(ajutor).mw-parser-output cite.citation{font-style:inherit}.mw-parser-output .citation q{quotes:"""""""'""'"}.mw-parser-output .citation .cs1-lock-free a{background:url("//upload.wikimedia.org/wikipedia/commons/thumb/6/65/Lock-green.svg/9px-Lock-green.svg.png")no-repeat;background-position:right .1em center}.mw-parser-output .citation .cs1-lock-limited a,.mw-parser-output .citation .cs1-lock-registration a{background:url("//upload.wikimedia.org/wikipedia/commons/thumb/d/d6/Lock-gray-alt-2.svg/9px-Lock-gray-alt-2.svg.png")no-repeat;background-position:right .1em center}.mw-parser-output .citation .cs1-lock-subscription a{background:url("//upload.wikimedia.org/wikipedia/commons/thumb/a/aa/Lock-red-alt-2.svg/9px-Lock-red-alt-2.svg.png")no-repeat;background-position:right .1em center}.mw-parser-output .cs1-subscription,.mw-parser-output .cs1-registration{color:#555}.mw-parser-output .cs1-subscription span,.mw-parser-output .cs1-registration span{border-bottom:1px dotted;cursor:help}.mw-parser-output .cs1-ws-icon a{background:url("//upload.wikimedia.org/wikipedia/commons/thumb/4/4c/Wikisource-logo.svg/12px-Wikisource-logo.svg.png")no-repeat;background-position:right .1em center}.mw-parser-output code.cs1-code{color:inherit;background:inherit;border:inherit;padding:inherit}.mw-parser-output .cs1-hidden-error{display:none;font-size:100%}.mw-parser-output .cs1-visible-error{font-size:100%}.mw-parser-output .cs1-maint{display:none;color:#33aa33;margin-left:0.3em}.mw-parser-output .cs1-subscription,.mw-parser-output .cs1-registration,.mw-parser-output .cs1-format{font-size:95%}.mw-parser-output .cs1-kern-left,.mw-parser-output .cs1-kern-wl-left{padding-left:0.2em}.mw-parser-output .cs1-kern-right,.mw-parser-output .cs1-kern-wl-right{padding-right:0.2em}
^
Brown, M. E.; Schaller, E. L. (2007). „The Mass of Dwarf Planet Eris”. Science. 316 (5831): 1585. Bibcode:2007Sci...316.1585B. doi:10.1126/science.1139415. PMID 17569855.
^
Johnston, W. R. (30 decembrie 2008). „(136199) Eris and Dysnomia”. Johnston's Archive. Accesat în 12 aprilie 2012.
- ^ ab
Green, D. W. E. (4 octombrie 2005). „S/2005 (2003 UB313 ) 1”. IAU Circular. 8610. Accesat în 12 ianuarie 2012.
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