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Voyager 1 observation of Loki Patera and nearby lava flows and volcanic pits. Loki Patera on moon Io (artist's concept; 0:18). [1] Map of temperature and crust age of Loki Patera obtained by the Large Binocular Telescope. Loki Patera / ˈ l oʊ k i ˈ p æ t ə r ə / is the largest volcanic depression on Jupiter's moon Io, 202 kilometres (126 ...
Io, with two plumes erupting from its surface, Galileo image, June 1997. Volcanism on Io, a moon of Jupiter, is represented by the presence of volcanoes, volcanic pits and lava flows on the surface. Io's volcanic activity was discovered in 1979 by Linda Morabito, an imaging scientist working on Voyager 1. [1]
Jupiter moon Io volcanic activity (left: December 14, 2022; right: March 1, 2023) This is a list of named volcanic surface features on Jupiter's moon Io. These names have been approved for use by the International Astronomical Union. The features listed below represent a subset of the total known volcanic features on Io's surface with the ...
These volcanic mountains are often smaller than the average mountain on Io, averaging only 1 to 2 km (0.6 to 1.2 mi) in height and 40 to 60 km (25 to 37 mi) wide. Other shield volcanoes with much shallower slopes are inferred from the morphology of several of Io's volcanoes, where thin flows radiate out from a central patera, such as at Ra Patera .
Amirani is about the same age as Jupiter, which is around 4.5 billion years old.It is surrounded by the Gish Bar Patera. [4] Within the mountains of the crater, Amirani lies at the center of a frozen sulphuric lava field that consists of a half-circle shaped, 37 kilometer wide volcanic pit, which is connected to a 330 kilometer compound lava flow by a narrow channel.
Colour image of Io's trailing hemisphere, highlighting the large red ring around the volcano Pele Pele is an active volcano on the surface of Jupiter 's moon Io . It is located on Io's trailing hemisphere at 18°42′S 255°18′W / 18.7°S 255.3°W / -18.7; -255
The thrust faulting and uplifting of large crust blocks on Io are interpreted by a model proposed by Schenk and Bulmer's 1998 paper. [3] In the model, Io's crust keeps recycling. Violent volcanic activity brings lava to the surface and older, buried layers are forced to subside. The old volcanic crust materials are compressed laterally as they ...
On Venus, volcanic features are very numerous and quite diverse, but, like on Mars, none are known to be currently active. These volcanoes range from several to several hundred kilometers in diameter; a majority of them are shield volcanoes. In addition, Venus has unusual types of volcanoes: pancake domes and scalloped margin domes. Most small ...