Evaporite karst in three interior layered deposits in Iani Chaos, Mars

Baioni, Davide; Tramontana, Mario

doi:10.1016/j.geomorph.2015.05.018

Cited by 14 publications

(9 citation statements)

References 58 publications

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“…4F). Additionally, they display strong morphological convergence with the evaporite dolines described in other regions of Mars, such as Tithonium Chasma (Baioni et al, 2009;Baioni & Wezel, 2010;Baioni 2013), Coprates Chasma (Baioni et al, 2011), Hebes Chasma (Grindrod & Balme, 2010;Jackson et al, 2011), Sinus Meridiani (Baioni & Sgavetti, 2013;Baioni et al, 2014;Flahaut et al, 2015), Iani Chaos (Baioni & Tramontana, 2015) and other regions (McKey & Nedell, 1998;Schaeffer, 1990;Spencer & Fanale, 1990).…”

Section: Interpretation Of the Karst Origin Of The Depressionsmentioning

confidence: 76%

“…Recent works based on new high-resolution images demonstrate the presence of karst landforms such as doline depressions in several Martian evaporite deposits (Baioni et al, 2009;Baioni & Wezel, 2010;Grindrod & Balme, 2010;Jackson et al, 2011;Flahaut et al, 2015), highlighting the usefulness of karst landforms as lithological, stratigraphic and paleoclimatic markers (Baioni & Sgavetti, 2013;Baioni & Tramontana, 2015).…”

Section: Introductionmentioning

confidence: 99%

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Possible evaporite karst in an interior layered deposit in Juventae Chasma, Mars

Baioni¹,

Tramontana²

2017

IJS

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Abstract:This paper describes karst landforms observed in an interior layered deposit (ILD) located within Juventae Chasma a trough of the Valles Marineris, a rift system that belongs to the Tharsis region of Mars. The ILD investigated is characterized by spectral signatures of kieserite, an evaporitic mineral present on Earth. A morphologic and morphometric survey of the ILD surface performed on data of the Orbiter High Resolution Imaging Science Experiment (HiRISE) highlighted the presence of depressions of various shapes and sizes. These landforms interpreted as dolines resemble similar karst landforms on Earth and in other regions of Mars. The observed karst landforms suggest the presence of liquid water, probably due to ice melting, in the Amazonian age.Mars, interior layered deposits, karst, climate change

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Section: Interpretation Of the Karst Origin Of The Depressionsmentioning

confidence: 76%

Section: Introductionmentioning

confidence: 99%

Possible evaporite karst in an interior layered deposit in Juventae Chasma, Mars

Baioni¹,

Tramontana²

2017

IJS

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“…Additionally, they strongly resemble the evaporite dolines described in other regions of Mars (Tab. 1), such as Tithonium Chasma (Baioni & wezel 2008;Baioni et al 2009;Baioni 2013), Coprates Chasma (Baioni et al 2011), Hebes Chasma (Grindrod & Balme 2010;Jackson et al 2011), Sinus Meridiani (Baioni & Sgavetti 2013;Flahaut et al 2015), Iani Chaos (Baioni & Tramontana 2015) and other regions (Schaeffer 1990;Spencer & Fanale 1990;McKey & Nedell 1998).…”

Section: Karst Landformsmentioning

confidence: 99%

Karst landforms Within Noctis Labyrinthus, Mars

Hajna¹,

Baioni

Tramontana

2017

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Noctis Labyrinthus je zapleten sistem pozno hesperijskih in zgodnje amazonijskih linearnih jarkov in krožnih globeli, ki povezuje vulkanski plato Tharsis in zahodni del Valles Marinerisa ob Marsovem ekvatorju. Ta študija je bila osredotočena na tri svetlo tonirane usedline (LTDs), ki se nahajajo v dnu jarka v zahodnem delu Noctis Labyrinthusa, s središčem območja na −6.8° N, 261.1° E, velikega približno 60 x 50 km in globino 5 km pod površjem bližnjega platoja. Te LTDs kamnine, ki se nahajajo na tleh v osrednjem območju tega jarka, izkazujejo spektralni zapis sadre, na njih je značilna prisotnost številnih plitvih depresij. Izvedli smo morfološke in morfometrične analize površin teh LTDs kamnin in to preko celostne študije slik visoke ločljivosti, ki so na voljo prek Marsovega Orbiterja (Reconnaissance Mars Orbiter High-Resolution Imaging Science Experiment) z namenom, da prvič opišemo ta površja, da razpravljamo o njihovem morebitnem izvoru ter njihovemu litološkemu in paleoklimatskemu pomenu. Analiza je na podlagi značilnosti preiskovanih reliefnih oblik in podobnosti z reliefnimi oblikami na Zemlji in Marsu ter zavržku drugih možnih izvorov pokazala, da so preiskane reliefne oblike na Marsu kraškega izvora. Zdi se, da preučevane oblike površja odražajo procese povezane z vodo, ki je najbrž nastajala zaradi taljenja ledu, tvorjenega v obdobjih bogatega odlaganja ledeno-snežnih plasti iz atmosfere, kot posledica sprememb v nagnjenosti osi Marsa, kar bi lahko povzročilo procese raztapljanja ali razpadanja na evaporitnih kamninah. Posledično opazovane kraške reliefne oblike kažejo na podnebne spremembe in prisotnost tekoče vode zaradi taljenja ledu v času poznega amazonija.

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“…These authors proposed that the observed variable degree of karst development could be related to variations in the solubility of different lithological units. Baioni and Tramontana (2015) documented putative sinkholes related to dissolution of sulphate-bearing layered deposits in Iani Chaos. Their interpretation was mainly based on the morphological analogy with terrestrial sinkholes and a discard analysis considering other potential genetic mechanisms.…”

Section: Introductionmentioning

confidence: 99%