Dorsa Stille

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Dorsa Stille is a wrinkle ridge system at 27°00′N19°00′W / 27.0°N 19.0°W / 27.0; -19.0 in Mare Imbrium on the Moon. It is 66 km long and was named after German geologist Hans Stille in 1976. [1]

Wrinkle ridge ridge, feature commonly found on lunar maria

A wrinkle ridge is a type of feature commonly found on lunar maria. These features are low, sinuous ridges formed on the mare surface that can extend for up to several hundred kilometers. Wrinkle ridges are tectonic features created when the basaltic lava cooled and contracted. They frequently outline ring structures buried within the mare, follow circular patterns outlining the mare, or intersect protruding peaks. They are sometimes called veins due to their resemblance to the veins that protrude from beneath the skin. These are found near craters.

Mare Imbrium vast lunar mare filling a basin on Earths Moon

Mare Imbrium is a vast lava plain within the Imbrium Basin on the Moon and is one of the larger craters in the Solar System. The Imbrium Basin formed from the collision of a proto-planet during the Late Heavy Bombardment. Basaltic lava later flooded the giant crater to form the flat volcanic plain seen today. The basin's age has been estimated using uranium–lead dating methods to 3938 ± 4 million years ago, the diameter of the impactor has been estimated to be 250 ± 25 km. The Moon's maria have fewer features than other areas of the Moon because molten lava pooled in the craters and formed a relatively smooth surface. Mare Imbrium is not as flat as it was originally because later events have altered its surface.

Moon Earths natural satellite

The Moon is an astronomical body that orbits planet Earth and is Earth's only permanent natural satellite. It is the fifth-largest natural satellite in the Solar System, and the largest among planetary satellites relative to the size of the planet that it orbits. The Moon is after Jupiter's satellite Io the second-densest satellite in the Solar System among those whose densities are known.

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Hans Stille A German ocean geologist known for alternative mechanisms of plate tectonics

Hans Wilhelm Stille was an influential German geologist working primarily on tectonics and the collation of tectonic events during the Phanerozoic. Stille adhered to the contracting Earth hypothesis and together with Leopold Kober he worked on the geosyncline theory to explain orogeny. Stille's ideas emerged in the aftermath of Eduard Suess' book Das Antlitz der Erde (1883–1909). Stille's and Kober's school of thought was one of two that emerged in the post-Suess era the other being headed by Alfred Wegener and Émile Argand. This competing view rejected Earth contraction and argued for continental drift. As Stille opposed continental drift he came to be labelled a "fixist".

Dorsa Andrusov wrinkle ridge

Dorsa Andrusov is a wrinkle ridge system at 1.0°S 57.0°E in Mare Fecunditatis on the Moon. It is 160 km in diameter and was named after Soviet geologist Nicolai Ivanovich Andrusov in 1976 by the IAU.

Dorsa Argand wrinkle ridge

Dorsa Argand is a wrinkle ridge system at 28.1°N 40.6°W on the Moon, in Oceanus Procellarum near the border with Mare Imbrium. It is approximately 92 km long and was named after Swiss geologist Émile Argand in 1976. The name of the feature was approved by the IAU in 1976.

Dorsa Barlow wrinkle ridge

Dorsa Barlow is a wrinkle ridge system on the Moon, in Mare Tranquilitatis near the border with Mare Serenitatis, centered at 14.0°N 30.6°E. It is about 110 km long and was named after British crystallographer William Barlow in 1976.

Dorsa Smirnov wrinkle ridge

Dorsa Smirnov is a wrinkle ridge system at 27.3°N 25.3°E in eastern Mare Serenitatis on the Moon. It is 222 km long and was named after Soviet geologist Sergei Sergeevich Smirnov by the IAU in 1976.

Dorsa Burnet wrinkle ridge

Dorsa Burnet are wrinkle ridges at 28.4°N 57.0°W in Oceanus Procellarum on the Moon. They are about 194 km long and were named after Thomas Burnet by the IAU in 1976.

Dorsa Cato wrinkle ridge

Dorsa Cato is a wrinkle ridge at 1.0°N 47.0°E on the Moon. It is approximately 130 km long and was named after Roman geological engineer Cato the Elder in 1976 by the IAU.

Dorsa Dana is a wrinkle ridge at 3.0°N 90.0°E in Mare Smythii on the Moon. It is 82 km long and was named after American geologist James Dwight Dana in 1976.

Dorsa Harker is a wrinkle ridge at 14.5°N 64.0°E in Mare Crisium on the Moon. It is 213 km long and was named after Alfred Harker, an English petrologist, in 1976.

Dorsa Mawson wrinkle ridge

Dorsa Mawson is a wrinkle ridge system at 7.0°S 53.0°E in Mare Fecunditatis on the Moon. It is approximately 143 km long and was named after Antarctic explorer Douglas Mawson in 1979 by the IAU.

Dorsa Rubey wrinkle ridge

Dorsa Rubey is a wrinkle ridge system at 10.0°S 42.0°W in Oceanus Procellarum on the Moon. It is 100 km long and was named after American geologist William Walden Rubey in 1976.

Dorsa Sorby wrinkle ridge

Dorsa Sorby is a wrinkle ridge system at 19.0°N 14.0°E in Mare Serenitatis on the Moon. It is 76 km long and was named after British geologist Henry Clifton Sorby in 1976.

Dorsa Tetyaev wrinkle ridge

Dorsa Tetyaev is a wrinkle ridge system at 19.9°N 64.2°E in Mare Crisium on the Moon. It is 188 km long and was named after Soviet geologist Mikhail Mikhailovich Tetyaev in 1979.

Dorsum Nicol wrinkle ridge

Dorsum Nicol is a wrinkle ridge on the Moon at 18.0°N 23.0°E in Mare Serenitatis near the border of Mare Tranquilitatis. It is 44 km long and was named after Scottish physicist William Nicol in 1976.

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References

  1. "Dorsa Stille" . Gazetteer of Planetary Nomenclature. USGS Astrogeology Research Program.