{{Short description|Geomorphological feature of the planet Mars}} {{use dmy dates|date=December 2015}} {{Infobox feature on celestial object |name = Aromatum Chaos |image = [[Image:Ravi Vallis.jpg|350px]] |caption = Aromatum Chaos and Ravi Vallis, as seen by Viking Orbiter |type = [[Chaotic terrain]] |location = [[Mars]] |coordinates = {{coord|1.09|S|317.0|E|globe:mars_type:landmark|display=inline,title}} |dimensions = {{convert|91.5|km|mi|abbr=on}} by {{convert|30|km|mi|abbr=on}} }} '''Aromatum Chaos''' is a deep depression, in what is considered [[chaotic terrain]]. It is the source of the [[outflow channel]] [[Ravi Vallis]], and is situated at the eastern end of Xanthe Terra, in the [[Margaritifer Sinus quadrangle]] (MC-19) region of [[Mars]], located at {{coord|1.09|S|317.0|E|globe:mars}}. Aromatum Chaos is {{convert|91.5|km|mi|abbr=on}} in length, and has an average width of about {{convert|30|km|mi|abbr=on}}.<ref name="JGR-20060817">{{cite journal |last1=Leask |first1=Harald J. |last2=Wilson |first2=Lionel |last3=Mitchell |first3=Karl L. |title=Formation of Aromatum Chaos, Mars: Morphological development as a result of volcano-ice interactions|date=17 August 2006 |journal=[[Journal of Geophysical Research]] |volume=111 |issue=E8 |pages=E08071 |doi=10.1029/2005JE002549 |bibcode=2006JGRE..111.8071L |url=https://eprints.lancs.ac.uk/id/eprint/8791/1/jgre2067.pdf |doi-access=free }}</ref><ref name="JGR-20060613">{{cite journal |last1=Leask |first1=Harald J. |last2=Wilson |first2=Lionel |last3=Mitchell |first3=Karl L. |title=Formation of Ravi Vallis outflow channel, Mars: Morphological development, water discharge, and duration estimates |date=13 June 2006 |journal=[[Journal of Geophysical Research]] |volume=111 |issue=E8 |pages=E08070 |doi=10.1029/2005JE002550 |bibcode=2006JGRE..111.8070L |url=https://eprints.lancs.ac.uk/id/eprint/8797/1/jgre2068.pdf |doi-access=free }}</ref><ref>{{cite web|url=http://planetarynames.wr.usgs.gov|title=Planetary Names: Welcome}}</ref><ref>{{cite web|url=http://themis.asu.edu/node/5622|title=A Flash In the Valley}}</ref>

The maximum depth of the floor of Aromatum Chaos has been calculated to be about {{convert|3.45|km|mi|abbr=on}} below the rim level. The mean depth of the western two-thirds of the Aromatum Chaos depression is about 1.64&nbsp;km, and the remaining eastern one third of the area, is estimated to be about {{val|1.2|0.05}} km in depth below the rim (using MOLA topography data). Thus, the average depth is {{convert|1.49|km|mi|abbr=on}}.<ref name="JGR-20060817" /><ref name="JGR-20060613" />

The Aromatum Chaos depression and the neighboring [[Ravi Vallis]] outflow channel are thought to have been caused by volcano-ice interactions, involving a combination of [[Levee|dikes]] and [[sill (geology)|sill]]s, which disrupted the [[cryosphere]] underneath the surface. This is thought to have pierced an underground [[aquifer]], resulting in the release of large amounts of water. This in turn caused crustal collapse, which created the Aromatum Chaos depression, and a catastrophic flood event, which formed the Ravi Vallis outflow channel. The flood has been estimated to have lasted between 2 and 10 weeks.<ref name="JGR-20060817" /><ref name="JGR-20060613" /> For estimates of water flow, such as the water speed, the volume discharge rate, and the minimum total water volume discharged, see the [[Ravi Vallis]] page.

Volcano-Ice interactions which took place at Aromatum Chaos, and the resulting catastrophic flood events which formed the neighboring Ravi Vallis outflow channel, are also known to have taken place in other parts of Mars, e.g.; [[Kasei Valles]],<ref>Keskea, A., C. Hamilton, A. McEwen, I. Daubar. Episodes of fluvial and volcanic activity in Mangala Valles, Mars. Icarus:245, 333-347.</ref> and [[Mangala Valles]].<ref name="JGR-20070224">{{cite journal |last1=Leask |first1=Harald J. |last2=Wilson |first2=Lionel |last3=Mitchell |first3=Karl L.|s2cid=14798124 |title=Formation of Mangala Fossa, the source of the Mangala Valles, Mars: Morphological development as a result of volcano-cryosphere interactions |date=24 February 2007 |journal=[[Journal of Geophysical Research]] |volume=112 |issue=E02011 |pages=E02011 |doi=10.1029/2005JE002644 |bibcode=2007JGRE..112.2011L |url=https://eprints.lancs.ac.uk/id/eprint/31116/1/2005JE002644.pdf |doi-access=free }}</ref><ref name="JGR-20070804">{{cite journal |last1=Leask |first1=Harald J. |last2=Wilson |first2=Lionel |last3=Mitchell |first3=Karl L.|title=Formation of Mangala Valles outflow channel, Mars: Morphological development and water discharge and duration estimates |date=4 August 2007 |journal=[[Journal of Geophysical Research]] |volume=112 |issue=E08003 |pages=E08003 |doi=10.1029/2006JE002851 |bibcode=2007JGRE..112.8003L |url=https://eprints.lancs.ac.uk/id/eprint/31123/1/2006JE002851.pdf |doi-access=free }}</ref>

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==See also== {{Div col|colwidth=30em}} * [[Chaos terrain]] * [[List of areas of chaos terrain on Mars]] * [[Martian chaos terrain]] * [[Outburst flood]] * [[Outflow channels]] {{div col end}}

== References == {{reflist|30em}}

{{Geography of Mars}} {{Portal bar|Solar System}}

[[Category:Margaritifer Sinus quadrangle]] [[Category:Valleys and canyons on Mars]] [[Category:Chaotic terrains on Mars]]