Skinakas (hypothetical basin): Difference between revisions
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Importing Wikidata short description: "Structure on Mercury" |
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{{Short description|Structure on Mercury}} |
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{{Mercury crater data |
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| latitude = 8 |
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| longitude = 280 |
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| E_or_W = W |
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{{Original research|date=October 2009}} |
{{Original research|date=October 2009}} |
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{{Infobox feature on celestial object |
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The '''Skinakas Basin''' is the informal name given to a structure on [[mercury (planet)|Mercury]] that appeared to be an extremely large [[impact basin]]. The traditional name for this region of Mercury is '''Solitudo Aphrodites'''.{{Citation needed|date=October 2008}} The limited-resolution images available showed a double-ringed structure, with the inner ring having a diameter of around 1600 km, which would have made it one of the largest impact basins in the [[solar system]]. It appeared to be even larger than the [[Caloris Basin]] on Mercury, which has been known since the [[Mariner 10]] flybys of that planet. The part of the outer ring that was imaged appeared to correspond to a diameter of around 2300 km.<ref name=Ksa06>{{cite journal|author = L. V. Ksanfomality|title= ''Earth-based optical imaging of Mercury''| journal= Advances in Space Research |volume= 38|issue = 4|pages= 594|year= 2006|bibcode= 2006AdSpR..38..594K|doi= 10.1016/j.asr.2005.05.071}}</ref> |
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| name = Skinakas |
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| location = [[Mercury (planet)|Mercury]] |
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| coordinates = {{coord|8|N|280|W|globe:mercury_type:landmark|display=inline,title}} |
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The basin |
The '''Skinakas basin''' is the informal name given to a structure on [[mercury (planet)|Mercury]] that appeared to be an extremely large [[impact basin]]. The limited-resolution ''[[Mariner 10]]'' images available showed a double-ringed structure, with the inner ring having a diameter of around 1600 km, which would have made it one of the largest impact basins in the [[Solar System]]. It appeared to be even larger than the [[Caloris Planitia|Caloris]] basin on Mercury, which has been known since the ''Mariner 10'' flybys of that planet. The part of the outer ring that was imaged appeared to correspond to a diameter of around 2300 km.<ref name=Ksa06>{{cite journal|author = L. V. Ksanfomality|title= ''Earth-based optical imaging of Mercury''| journal= Advances in Space Research |volume= 38|issue = 4|pages= 594|date= 2006|bibcode= 2006AdSpR..38..594K|doi= 10.1016/j.asr.2005.05.071}}</ref> |
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However, images returned during the inbound phase of the 6 October 2008 fly-by of Mercury by NASA's [[MESSENGER]] spacecraft showed conclusively that the Skinakas basin is illusory.{{Citation needed|date=June 2009}} |
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The basin was supposedly centered at about {{Coord|8|N|80|E|globe:mercury}}<ref name=Fassett_2012/> and lay on the hemisphere of Mercury that was not imaged by ''[[Mariner 10]]''. This place is situated near an [[List of albedo features on Mercury|albedo feature]] Solitudo Aphrodites ({{Coord|25|N|70|E|globe:mercury}}).<ref>{{GPN|5628|Solitudo Aphrodites}}</ref> In 2001, it was observed and imaged by ALPO ([[Association of Lunar and Planetary Observers]]) members.{{Citation needed|date=October 2008}} But it was followed by L. Ksanfomality from [[lucky imaging]] observations in 2004. The informal name is after the [[Skinakas Observatory|Skinakas observatory]] on [[Crete]] where the observations were taken.<ref name=Ksa06/> Despite radar images having a far greater resolution they are not useful for detecting very large impact basins such as this one; for example, the Caloris basin is also not visible in radar.<ref name=HarSlaBut07>{{cite journal|author=J. K. Harmon|display-authors=etal|title=''Mercury: Radar images of the equatorial and midlatitude zones''|journal=Icarus|volume=187|issue=2|pages=374|date=2007|bibcode=2007Icar..187..374H|doi=10.1016/j.icarus.2006.09.026}}</ref> |
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However, careful examination of images by ''[[MESSENGER]]'' spacecraft showed no evidence of the Skinakas basin.<ref name=Fassett_2012/> |
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==References== |
==References== |
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{{reflist |
{{reflist|refs= |
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<ref name=Fassett_2012>{{cite journal |
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|author=Fassett C. I. |author2=Head J. W. |author3=Baker D. M. H. |display-authors=etal |
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|date=2012 |
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|title=Large impact basins on Mercury: Global distribution, characteristics, and modification history from MESSENGER orbital data |
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|journal=Journal of Geophysical Research |
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|volume=117 |
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|issue=E12 |
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|doi=10.1029/2012JE004154 |
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|bibcode=2012JGRE..117.0L08F |
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|url=http://www.planetary.brown.edu/pdfs/4324.pdf |
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|archiveurl=https://web.archive.org/web/20130129075452/http://www.planetary.brown.edu/pdfs/4324.pdf |
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|archivedate=2013-01-29 |
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}}</ref> |
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}} |
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{{Mercury (planet)}} |
{{Mercury (planet)}} |
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[[Category:Surface features of Mercury]] |
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[[Category:Mercury (planet)]] |
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Latest revision as of 00:20, 28 June 2024
 | This article possibly contains original research. (October 2009) |
| Location | Mercury |
|---|---|
| Coordinates | 8°N 280°W / 8°N 280°W |
| Diameter | 2300 km |
| Eponym | Skinakas observatory |
The Skinakas basin is the informal name given to a structure on Mercury that appeared to be an extremely large impact basin. The limited-resolution Mariner 10 images available showed a double-ringed structure, with the inner ring having a diameter of around 1600 km, which would have made it one of the largest impact basins in the Solar System. It appeared to be even larger than the Caloris basin on Mercury, which has been known since the Mariner 10 flybys of that planet. The part of the outer ring that was imaged appeared to correspond to a diameter of around 2300 km.[1]
The basin was supposedly centered at about 8°N 80°E / 8°N 80°E[2] and lay on the hemisphere of Mercury that was not imaged by Mariner 10. This place is situated near an albedo feature Solitudo Aphrodites (25°N 70°E / 25°N 70°E).[3] In 2001, it was observed and imaged by ALPO (Association of Lunar and Planetary Observers) members.[citation needed] But it was followed by L. Ksanfomality from lucky imaging observations in 2004. The informal name is after the Skinakas observatory on Crete where the observations were taken.[1] Despite radar images having a far greater resolution they are not useful for detecting very large impact basins such as this one; for example, the Caloris basin is also not visible in radar.[4] However, careful examination of images by MESSENGER spacecraft showed no evidence of the Skinakas basin.[2]
References
[edit]- ^ a b L. V. Ksanfomality (2006). "Earth-based optical imaging of Mercury". Advances in Space Research. 38 (4): 594. Bibcode:2006AdSpR..38..594K. doi:10.1016/j.asr.2005.05.071.
- ^ a b Fassett C. I.; Head J. W.; Baker D. M. H.; et al. (2012). "Large impact basins on Mercury: Global distribution, characteristics, and modification history from MESSENGER orbital data" (PDF). Journal of Geophysical Research. 117 (E12). Bibcode:2012JGRE..117.0L08F. doi:10.1029/2012JE004154. Archived from the original (PDF) on 2013-01-29.
- ^ "Solitudo Aphrodites". Gazetteer of Planetary Nomenclature. USGS Astrogeology Research Program.
- ^ J. K. Harmon; et al. (2007). "Mercury: Radar images of the equatorial and midlatitude zones". Icarus. 187 (2): 374. Bibcode:2007Icar..187..374H. doi:10.1016/j.icarus.2006.09.026.
