Editing Titan (moon) (section)

=== Tectonics and cryovolcanism ===
Through ''Cassini'' RADAR mapping of Titan's surface, numerous landforms have been interpreted as candidate [[cryovolcanic]] and [[tectonic]] features by multiple authors.<ref name="Liu 2016"/>{{rp|14}} A 2016 analysis of mountainous ridges on Titan revealed that ridges are concentrated in Titan's equatorial regions, implying that ridges either form more frequently in or are better preserved in low-latitude regions. The ridges—primarily oriented east to west—are linear to arcuate in shape, with the authors of the analysis comparing them to terrestrial [[fold belt]]s indicative of horizontal compression or convergence. They note that the global distribution of Titan's ridges could be indicative of global contraction, with a thickened ice shell causing regional uplift.<ref name="Liu 2016">{{cite journal |last1=Liu |first1=Zac Yung-Chun |display-authors=et al. |title=The tectonics of Titan: Global structural mapping from Cassini RADAR |date=May 2016 |journal=Icarus |volume=270 |pages=14–29 |doi=10.1016/j.icarus.2015.11.021 |bibcode=2016Icar..270...14L }}</ref>{{rp|23–25}}

The identification of cryovolcanic features on Titan remains controversial and inconclusive, primarily due to limitations of ''Cassini'' imagery and coverage. ''Cassini'' RADAR and VIMS imagery revealed several candidate cryovolcanic features, particularly flow-like terrains in western Xanadu and steep-sided lakes in the northern hemisphere that resemble [[maar]] craters on Earth, which are created by explosive subterranean eruptions. The likeliest cryovolcano features is a complex of landforms that includes two mountains, [[Doom Mons]] and [[Erebor Mons]]; a large depression, [[Sotra Patera]]; and a system of flow-like features, [[Mohini Fluctus]]. Between 2005 and 2006, parts of Sotra Patera and Mohini Fluctus became significantly brighter whilst the surrounding plains remained unchanged, potentially indicative of ongoing cryovolcanic activity.<ref name="Lopes2019">{{cite journal |last1=Lopes |first1=R. M. C. |title=Titan as Revealed by the Cassini Radar |date=June 2019 |journal=Space Science Reviews |volume=215 |issue=4 |page=33 |doi=10.1007/s11214-019-0598-6 |bibcode=2019SSRv..215...33L |hdl=11573/1560405 |hdl-access=free }}</ref>{{rp|21–23}} Indirect lines of evidence for cryovolcanism include the presence of Argon-40 in Titan's atmosphere. Radiogenic <sup>40</sup>Ar is sourced from the decay of [[Potassium-40|<sup>40</sup>K]], and has likely been produced within Titan over the course of billions of years within its rocky core. <sup>40</sup>Ar's presence in Titan's atmosphere is thus supportive of active geology on Titan, with cryovolcanism being one possible method of bringing the isotope up from the interior.<ref name="Niemann2005">{{cite journal |last1=Niemann |first1=H. B. |title=The abundances of constituents of Titan's atmosphere from the GCMS instrument on the Huygens probe |date=December 2005 |journal=Nature |volume=438 |issue=7069 |pages=779–784 |doi=10.1038/nature04122 |pmid=16319830 |bibcode=2005Natur.438..779N |hdl=2027.42/62703 |hdl-access=free }}</ref>