Copernicus (Martian crater)
Copernicus is a large crater on Mars , with a diameter close to 300 km. It is located south of the planet's equator in the heavily cratered highlands of Terra Sirenum in the Phaethontis quadrangle at 48.8°S and 191.2°E. [1] Its name was approved in 1973, and it was named after Nicolaus Copernicus .
Page Revisions
| Year | Metadata | Sections | Top Words | First Paragraph |
| 2018 |
87213 characters 6 sections 9 paragraphs 8 images 659 internal links 12 external links |
copernicus 0.663 gullies 0.190 changes 0.188 ctx 0.153 dry 0.134 dust 0.131 frost 0.126 crater 0.124 eastern 0.116 dikes 0.113 devils 0.109 coating 0.105 nordenskiöld 0.101 liquid 0.100 devil 0.099 |
Copernicus is a large crater on Mars , with a diameter close to 300 km. It is located south of the planet's equator in the heavily cratered highlands of Terra Sirenum in the Phaethontis quadrangle at 48.8°S and 191.2°E. [1] Its name was approved in 1973, and it was named after Nicolaus Copernicus . |
|
| 2017 |
45875 characters 6 sections 9 paragraphs 11 images 167 internal links 12 external links |
copernicus 0.663 gullies 0.190 changes 0.188 ctx 0.153 dry 0.134 dust 0.131 frost 0.126 crater 0.124 eastern 0.116 dikes 0.113 devils 0.109 coating 0.105 nordenskiöld 0.101 liquid 0.100 devil 0.099 |
Copernicus is a large crater on Mars , with a diameter close to 300 km. It is located south of the planet's equator in the heavily cratered highlands of Terra Sirenum in the Phaethontis quadrangle at 48.8°S and 191.2°E. [1] Its name was approved in 1973, and it was named after Nicolaus Copernicus . |
|
| 2016 |
37850 characters 3 sections 6 paragraphs 10 images 153 internal links 9 external links |
copernicus 0.725 gullies 0.208 changes 0.205 ctx 0.167 dry 0.146 frost 0.138 eastern 0.127 dikes 0.123 crater 0.123 liquid 0.109 edge 0.107 reconnaissance 0.103 camera 0.097 water 0.087 floor 0.085 |
Copernicus is a large crater on Mars , with a diameter close to 300 km. It is located south of the planet's equator in the heavily cratered highlands of Terra Sirenum in the Phaethontis quadrangle at 48.8°S and 191.2°E. [1] Its name was approved in 1973, and it was named after Nicolaus Copernicus . The impact that formed Copernicus likely occurred more than 3 billion years ago. The crater contains smaller craters within its basin and is particularly notable for gully formations that are presumed to be indicative of past liquid water flows. Many small channels exist in this area; they are further evidence of liquid water. On the basis of their form, aspects, positions, and location amongst and apparent interaction with features thought to be rich in water ice, many researchers believed that the processes carving the gullies involve liquid water. However, this remains a topic of active research. As soon as gullies were discovered, [2] researchers began to image many gullies over and over, looking for possible changes. By 2006, some changes were found. [3] Later, with further analysis it was determined that the changes could have occurred by dry granular flows rather than being driven by flowing water. [4] [5] [6] With continued observations many more changes were found in Gasa Crater and others. [7] With more repeated observations, more and more changes have been found; since the changes occur in the winter and spring, experts are tending to believe that gullies were formed from dry ice. Before-and-after images demonstrated the timing of this activity coincided with seasonal carbon-dioxide frost and temperatures that would not have allowed for liquid water. When dry ice frost changes to a gas, it may lubricate dry material to flow especially on steep slopes. [8] [9] [10] In some years frost, perhaps as thick as 1 meter. |
|
| 2015 |
37773 characters 3 sections 6 paragraphs 10 images 153 internal links 9 external links |
copernicus 0.725 gullies 0.208 changes 0.205 ctx 0.167 dry 0.146 frost 0.138 eastern 0.127 dikes 0.123 crater 0.123 liquid 0.109 edge 0.107 reconnaissance 0.103 camera 0.097 water 0.087 floor 0.085 |
Copernicus is a large crater on Mars , with a diameter close to 300 km. It is located south of the planet's equator in the heavily cratered highlands of Terra Sirenum in the Phaethontis quadrangle at 48.8°S and 191.2°E. [1] Its name was approved in 1973, and it was named after Nicolaus Copernicus . The impact that formed Copernicus likely occurred more than 3 billion years ago. The crater contains smaller craters within its basin and is particularly notable for gully formations that are presumed to be indicative of past liquid water flows. Many small channels exist in this area; they are further evidence of liquid water. On the basis of their form, aspects, positions, and location amongst and apparent interaction with features thought to be rich in water ice, many researchers believed that the processes carving the gullies involve liquid water. However, this remains a topic of active research. As soon as gullies were discovered, [2] researchers began to image many gullies over and over, looking for possible changes. By 2006, some changes were found. [3] Later, with further analysis it was determined that the changes could have occurred by dry granular flows rather than being driven by flowing water. [4] [5] [6] With continued observations many more changes were found in Gasa Crater and others. [7] With more repeated observations, more and more changes have been found; since the changes occur in the winter and spring, experts are tending to believe that gullies were formed from dry ice. Before-and-after images demonstrated the timing of this activity coincided with seasonal carbon-dioxide frost and temperatures that would not have allowed for liquid water. When dry ice frost changes to a gas, it may lubricate dry material to flow especially on steep slopes. [8] [9] [10] In some years frost, perhaps as thick as 1 meter. |