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Irnini Mons
Irnini Mons is a volcanic structure on the planet Venus, and is named after the Assyro-Babylonian goddess of cedar-tree mountains.〔"Irnini Mons." ''Gazetteer of Planetary Nomenclature''. USGS. Web. 23 Feb. 2014 (http://planetarynames.wr.usgs.gov )〕 It has a diameter of , a height of , and is located in Venus' northern hemisphere.〔Matiella Novak, M.A.; Buczkowski, D.L. (2012). Structural mapping around Irnini Mons, Venus. 43rd Lunar and Planetary Science Conference. LPI. Abstract 2070. http://www.lpi.usra.edu/meetings/lpsc2012/pdf/2070.pdf〕 More specifically, it is located in the central Eistla Regio region at () in the V-20 quadrangle.〔 Sappho Patera, a diameter wide, caldera-like, depression tops the summit of Irnini Mons.〔Matiella Novak, M.A.; Buczkowski, D.L. (2014). Determining relative ages of structural features around Irnini Mons, Venus - A comparison of four type locations to resolve the timing of cross cutting features. 45th Lunar and Planetary Science Conference. LPI. Abstract 2569. http://www.hou.usra.edu/meetings/lpsc2014/pdf/2569.pdf〕 The primary structural features surrounding Irnini Mons are graben, seen as linear depressed sections of rock, radiating from the central magma chamber. Also, concentric, circular ridges and graben outline the Sappho Patera depression at the summit. The volcano is crossed by various rift zones, including the north-south trending Badb Linea rift, the Guor Linea rift extending to the northwest, and the Virtus Linea rift continuing to the southeast.〔
The combination of volcanic-tectonic structures around Irnini Mons supports varying intensities of deformation and a multi-directional stress history. Although classified as a shield volcano, Irnini Mons contains many elements of the Venusian coronae, bringing speculation to its formation. If Irnini Mons was originally a corona, a shallow oval-shaped depression, it would support a thin lithosphere on Venus. On the other hand, it being a shield volcano supports the theory of a thicker lithosphere and Irnini Mons' stress history could be summarized simply as a transition from predominantly compressive forces to extensional relaxation, resulting in the observed radiating graben and concentric ridges.〔
Irnini Mons is a significant structural feature on Venus because the preservation of the geology allows for the analysis of Venus' regional stress orientation in response to a pressurized magma chamber over time.〔Buczkowski, D.L.; McGill, G.E.; Cooke, M.L. (2004). Anomalous radial strcutures at Irnini Mons, Venus: A parametric study of stresses on a pressurized hole. 35th Lunar and Planetary Science Conference. LPI. Abstract 1561. http://www.lpi.usra.edu/meetings/lpsc2004/pdf/1561.pdf〕
==Geology of Irnini Mons==
The geology of Irnini Mons and the surrounding region was interpreted using synthetic aperture radar data from the Magellan space mission. Stratigraphic units were identified using their relative brightness and texture. Topography and structural features, such as cross-cutting relationships, were also taken into account.〔McGill, George. Geologic map of the Sappho Patera quadrangle (V-20), Venus. USGS. US Department of the Interior. Map I-2637. http://pubs.usgs.gov/imap/2637/pdf/I2637pamphlet.pdf〕 The extremely low erosional rates on Venus contribute to the preservation of many of these volcanic-tectonic features. The high pressure inhibits wind erosion, the dryness prevents water erosion, and the lack of volatiles in magma results in structures that are mostly untouched.〔Kostama, V.P. "The crowns, spiders, and stars of Venus: Characterization and assessment of the geologic settings of volcano-tectonic structures on Venus." ''Report Series in Physical Sciences''. Report 42. University of Oulu, Finland. GEOREF. Web. 26 Feb 2014. http://herkules.oulu.fi/isbn9514283171/isbn9514283171.pdf〕
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