Skinakas (hypothetical basin): Difference between revisions
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{{Original research|date=October 2009}} |
{{Original research|date=October 2009}} |
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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|pages= 594|year= 2006| |
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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The basin was supposedly centered at about 280°W, 8° N, and lay on the hemisphere of Mercury that was not imaged by [[Mariner 10]]. In 2001, it was observed and imaged by ALPO ([[Association of Lunar and Planetary Observers]]) members.{{Citation needed|date=October 2008}} It was then known as Solitudo Aphrodites. But it was followed by L. Ksanfomality from [[lucky imaging]] observations in 2004. The informal name is after the [[Mount Ida, Crete|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 ''et al.''|title=''Mercury: Radar images of the equatorial and midlatitude zones''|journal=Icarus|volume=187|pages=374|year=2007| |
The basin was supposedly centered at about 280°W, 8° N, and lay on the hemisphere of Mercury that was not imaged by [[Mariner 10]]. In 2001, it was observed and imaged by ALPO ([[Association of Lunar and Planetary Observers]]) members.{{Citation needed|date=October 2008}} It was then known as Solitudo Aphrodites. But it was followed by L. Ksanfomality from [[lucky imaging]] observations in 2004. The informal name is after the [[Mount Ida, Crete|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 ''et al.''|title=''Mercury: Radar images of the equatorial and midlatitude zones''|journal=Icarus|volume=187|issue=2|pages=374|year=2007|bibcode=2007Icar..187..374H|doi=10.1016/j.icarus.2006.09.026}}</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}} |
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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Revision as of 13:03, 15 March 2011
 | This article possibly contains original research. (October 2009) |
The Skinakas Basin is the informal name given to a structure on Mercury that appeared to be an extremely large impact basin. The traditional name for this region of Mercury is Solitudo Aphrodites.[citation needed] 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.[1]
The basin was supposedly centered at about 280°W, 8° N, and lay on the hemisphere of Mercury that was not imaged by Mariner 10. In 2001, it was observed and imaged by ALPO (Association of Lunar and Planetary Observers) members.[citation needed] It was then known as Solitudo Aphrodites. 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.[2] 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]
References
- ^ 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.
- ^ 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.
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