Page Revisions
| Year | Metadata | Sections | Top Words | First Paragraph |
| 2018 |
76946 characters 3 sections 5 paragraphs 2 images 653 internal links 4 external links |
yuty 0.752 ejecta 0.289 craters 0.164 rampart 0.143 complex 0.138 morphology 0.138 lobes 0.103 terminology 0.102 splosh 0.093 subsurface 0.089 characteristic 0.088 distinctive 0.085 paraguay 0.084 terracing 0.084 lobate 0.083 |
Yuty is a crater on Mars in Chryse Planitia , named after the town of Yuty in Paraguay. It measures approximately 19 kilometres (12 miles) in diameter, and is surrounded by complex ejecta lobes, which are a distinctive characteristic of martian impact craters. [1] [2] |
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| 2017 |
35370 characters 3 sections 5 paragraphs 5 images 159 internal links 3 external links |
yuty 0.752 ejecta 0.289 craters 0.164 rampart 0.143 complex 0.138 morphology 0.138 lobes 0.103 terminology 0.102 splosh 0.093 subsurface 0.089 characteristic 0.088 distinctive 0.085 paraguay 0.084 terracing 0.084 lobate 0.083 |
Yuty is a crater on Mars in Chryse Planitia , named after the town of Yuty in Paraguay. It measures approximately 19 kilometres (12 miles) in diameter, and is surrounded by complex ejecta lobes, which are a distinctive characteristic of martian impact craters. [1] [2] |
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| 2013 |
32592 characters 2 sections 4 paragraphs 5 images 157 internal links 1 external links |
yuty 0.716 ejecta 0.310 craters 0.176 rampart 0.153 complex 0.148 morphology 0.147 lobes 0.111 terminology 0.110 splosh 0.099 subsurface 0.096 characteristic 0.094 distinctive 0.091 crater 0.090 terracing 0.090 lobate 0.089 |
Yuty is a crater on Mars in Chryse Planitia . The crater is about 20 km (12 mi) in diameter, and is surrounded by complex ejecta lobes, which are a distinctive characteristic of martian impact craters. [1] Many craters at equatorial and mid-latitudes on Mars have this form of ejecta morphology, which is thought to arise when the impacting object melts ice in the subsurface. Liquid water in the ejected material forms a muddy slurry that flows along the surface, producing the characteristic lobe shapes. [2] [3] The presence of a pre-existing, partially buried crater on Yuty’s southwestern rim is evidence that the ejecta is thin. [4] |
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| 2011 |
12775 characters 2 sections 5 paragraphs 2 images 16 internal links 1 external links |
yuty 0.716 ejecta 0.310 craters 0.176 rampart 0.153 complex 0.148 morphology 0.147 lobes 0.111 terminology 0.110 splosh 0.099 subsurface 0.096 characteristic 0.094 distinctive 0.091 crater 0.090 terracing 0.090 lobate 0.089 |
Yuty is a crater on Mars in Chryse Planitia . The crater is about 20 km (12 mi) in diameter, and is surrounded by complex ejecta lobes, which are a distinctive characteristic of martian impact craters. [1] Many craters at equatorial and mid-latitudes on Mars have this form of ejecta morphology, which is thought to arise when the impacting object melts ice in the subsurface. Liquid water in the ejected material forms a muddy slurry that flows along the surface, producing the characteristic lobe shapes. [2] [3] The presence of a pre-existing, partially buried crater on Yuty’s southwestern rim is evidence that the ejecta is thin. [4] |
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| 2010 |
12700 characters 2 sections 5 paragraphs 2 images 15 internal links 1 external links |
yuty 0.717 ejecta 0.310 craters 0.176 rampart 0.154 complex 0.149 morphology 0.148 lobes 0.111 terminology 0.110 splosh 0.099 subsurface 0.096 characteristic 0.094 distinctive 0.091 crater 0.090 terracing 0.090 lobate 0.089 |
Yuty is a crater on Mars in Chryse Planitia . The crater is about 20 km (12.4 miles) in diameter, and is surrounded by complex ejecta lobes, which are a distinctive characteristic of martian impact craters [1] . Many craters at equatorial and mid-latitudes on Mars have this form of ejecta morphology, which is thought to arise when the impacting object melts ice in the subsurface. Liquid water in the ejected material forms a muddy slurry that flows along the surface, producing the characteristic lobe shapes [2] [3] . The presence of a pre-existing, partially buried crater on Yuty’s southwestern rim is evidence that the ejecta is thin [4] . |
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| 2009 |
8972 characters 2 sections 3 paragraphs 2 images 12 internal links 2 external links |
yuty 0.389 lobe 0.276 ejecta 0.269 melts 0.253 lobes 0.241 impacting 0.238 morphology 0.214 characteristic 0.204 partly 0.203 chryse 0.200 ejected 0.168 surrounded 0.160 equatorial 0.153 covers 0.149 shapes 0.147 |
The crater is about 18 km in diameter, and is surrounded by complex ejecta lobes, one of which partly covers an older crater. [1] Many craters at equatorial and mid-latitudes on Mars have this form of ejecta morphology, which is believed to arise when the impacting object melts ice in the subsurface. Liquid water in the ejected material would then allow it to flow, forming the characteristic lobe shapes. [2] |
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| 2008 |
8951 characters 2 sections 2 paragraphs 2 images 12 internal links 2 external links |
yuty 0.392 lobe 0.277 ejecta 0.271 melts 0.254 lobes 0.242 impacting 0.240 morphology 0.215 characteristic 0.205 partly 0.204 chryse 0.201 ejected 0.169 surrounded 0.161 equatorial 0.154 covers 0.150 shapes 0.148 |
The crater is about 18km in diameter, and is surrounded by complex ejecta lobes, one of which partly covers an older crater. [1] Many craters at equatorial and mid-latitudes on Mars have this form of ejecta morphology, which is believed to arise when the impacting object melts ice in the subsurface. Liquid water in the ejected material would then allow it to flow, forming the characteristic lobe shapes. [2] |
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| 2007 |
9026 characters 2 sections 2 paragraphs 2 images 13 internal links 2 external links |
yuty 0.389 lobe 0.275 ejecta 0.269 melts 0.252 lobes 0.240 impacting 0.238 morphology 0.213 characteristic 0.204 partly 0.202 chryse 0.200 crater 0.173 ejected 0.168 surrounded 0.160 equatorial 0.152 covers 0.149 |
The crater is about 18km in diameter, and is surrounded by complex ejecta lobes, one of which partly covers an older crater. [1] Many craters at equatorial and mid-latitudes on Mars have this form of ejecta morphology, which is believed to arise when the impacting object melts ice in the subsurface. Liquid water in the ejected material would then allow it to flow, forming the characteristic lobe shapes. [2] |