{"paper_id":"44ffe6ef-a92c-447e-b40d-00d2068e9b88","body_text":"High flow capacity and Low Viscosity of the Séítah Formation, at Jezero Crater, Mars | Research Square window.SnipcartSettings = { analytics: { enabled: false } }; (function() { var accessVector = localStorage.getItem('access_vector') || ''; window.dataLayer = window.dataLayer || []; if (accessVector) { window.dataLayer.push({ user: { profile: { profileInfo: { snid: accessVector } } } }); } })(); (function(w,d,s,l,i){w[l]=w[l]||[];w[l].push({'gtm.start':new Date().getTime(),event:'gtm.js'});var f=d.getElementsByTagName(s)[0],j=d.createElement(s),dl=l!='dataLayer'?'&l='+l:'';j.async=true;j.src='https://www.googletagmanager.com/gtm.js?id='+i+dl;f.parentNode.insertBefore(j,f);})(window,document,'script','dataLayer','GTM-K279D39R'); Browse Preprints In Review Journals COVID-19 Preprints AJE Video Bytes Research Tools Research Promotion AJE Professional Editing AJE Rubriq About Preprint Platform In Review Editorial Policies Our Team Advisory Board Help Center Sign In Submit a Preprint Cite Share Download PDF Article High flow capacity and Low Viscosity of the Séítah Formation, at Jezero Crater, Mars Adrian Brown, Linda Kah, Roger Wiens, Patrick Pinet, Arya Udry, and 23 more This is a preprint; it has not been peer reviewed by a journal. https://doi.org/ 10.21203/rs.3.rs-8742433/v1 This work is licensed under a CC BY 4.0 License Status: Under Review Version 1 posted You are reading this latest preprint version Abstract The unexpected discovery of olivine cumulate at the Séítah Formation within Jezero Crater was one of the most compelling findings of the Mars2020 Perseverance rover mission thus far. Compared to Earth, Mars is a basaltic world and differences in gravity, atmosphere and volatile content imply commensurate changes in lava flow dynamics that need to be better understood. We use rover geochemistry data to calculate the viscosity and relative flow distance of the Séítah unit and its parental lava. We suggest the olivine cumulate discovered by the rover was related to a ponded lava flow, based on the low viscosity and distribution of the unit. We estimate an approximate relative depth for the cumulate layer of the lava pond using a convective lava magma model. We also compare the Noachian Jezero olivine rich viscosities to Hesperian basalts analysed by Spirit, and find the Noachian samples to have a greater propensity to flow than their younger cousins. Future observations of the olivine rich unit and laboratory studies of the samples collected by Mars2020 will provide a deep window into the flow dynamics and evolution of Martian lava flows. Earth and environmental sciences/Planetary science/Volcanology Earth and environmental sciences/Planetary science/Inner planets Full Text Additional Declarations There is NO Competing Interest. Cite Share Download PDF Status: Under Review Version 1 posted You are reading this latest preprint version Research Square lets you share your work early, gain feedback from the community, and start making changes to your manuscript prior to peer review in a journal. As a division of Research Square Company, we’re committed to making research communication faster, fairer, and more useful. We do this by developing innovative software and high quality services for the global research community. Our growing team is made up of researchers and industry professionals working together to solve the most critical problems facing scientific publishing. Also discoverable on Platform About Our Team In Review Editorial Policies Advisory Board Help Center Resources Author Services Accessibility API Access RSS feed Manage Cookie Preferences © Research Square 2026 | ISSN 2693-5015 (online) Privacy Policy Terms of Service Do Not Sell My Personal Information {\"props\":{\"pageProps\":{\"initialData\":{\"identity\":\"rs-8742433\",\"acceptedTermsAndConditions\":true,\"allowDirectSubmit\":false,\"archivedVersions\":[],\"articleType\":\"Article\",\"associatedPublications\":[],\"authors\":[{\"id\":585194057,\"identity\":\"4b911ba6-deca-441f-82c8-85cad41d2c7d\",\"order_by\":0,\"name\":\"Adrian 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14:56:05\",\"currentVersionCode\":1,\"declarations\":\"\",\"doi\":\"10.21203/rs.3.rs-8742433/v1\",\"doiUrl\":\"https://doi.org/10.21203/rs.3.rs-8742433/v1\",\"draftVersion\":[],\"editorialEvents\":[],\"editorialNote\":\"\",\"failedWorkflow\":false,\"files\":[{\"id\":102295161,\"identity\":\"396f8a6d-f233-4880-9c89-a975a424650c\",\"added_by\":\"auto\",\"created_at\":\"2026-02-10 10:09:26\",\"extension\":\"pdf\",\"order_by\":1,\"title\":\"\",\"display\":\"\",\"copyAsset\":false,\"role\":\"manuscript-pdf\",\"size\":1708469,\"visible\":true,\"origin\":\"\",\"legend\":\"Article File\",\"description\":\"\",\"filename\":\"LowViscosityofSeitahFormation.pdf\",\"url\":\"https://assets-eu.researchsquare.com/files/rs-8742433/v1_covered_55a53d20-0736-464d-9f66-c3b96767fe72.pdf\"}],\"financialInterests\":\"There is \\u003cb\\u003eNO\\u003c/b\\u003e Competing Interest.\",\"formattedTitle\":\"High flow capacity and Low Viscosity of the Séítah Formation, at Jezero Crater, Mars\",\"fulltext\":[],\"fulltextSource\":\"\",\"fullText\":\"\",\"funders\":[],\"hasAdminPriorityOnWorkflow\":false,\"hasManuscriptDocX\":false,\"hasOptedInToPreprint\":true,\"hasPassedJournalQc\":\"\",\"hasAnyPriority\":false,\"hideJournal\":false,\"highlight\":\"\",\"institution\":\"\",\"isAcceptedByJournal\":false,\"isAuthorSuppliedPdf\":true,\"isDeskRejected\":\"\",\"isHiddenFromSearch\":false,\"isInQc\":false,\"isInWorkflow\":false,\"isPdf\":true,\"isPdfUpToDate\":true,\"isWithdrawnOrRetracted\":false,\"journal\":{\"display\":true,\"email\":\"info@researchsquare.com\",\"identity\":\"nature-portfolio\",\"isNatureJournal\":true,\"hasQc\":false,\"allowDirectSubmit\":false,\"externalIdentity\":\"\",\"sideBox\":\"\",\"snPcode\":\"\",\"submissionUrl\":\"\",\"title\":\"Nature 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Compared to Earth, Mars is a basaltic world and differences in gravity, atmosphere and volatile content imply commensurate changes in lava flow dynamics that need to be better understood. We use rover geochemistry data to calculate the viscosity and relative flow distance of the Séítah unit and its parental lava. We suggest the olivine cumulate discovered by the rover was related to a ponded lava flow, based on the low viscosity and distribution of the unit. We estimate an approximate relative depth for the cumulate layer of the lava pond using a convective lava magma model. We also compare the Noachian Jezero olivine rich viscosities to Hesperian basalts analysed by Spirit, and find the Noachian samples to have a greater propensity to flow than their younger cousins. Future observations of the olivine rich unit and laboratory studies of the samples collected by Mars2020 will provide a deep window into the flow dynamics and evolution of Martian lava flows.\",\"manuscriptTitle\":\"High flow capacity and Low Viscosity of the Séítah Formation, at Jezero Crater, Mars\",\"msid\":\"\",\"msnumber\":\"\",\"nonDraftVersions\":[{\"code\":1,\"date\":\"2026-02-05 11:48:23\",\"doi\":\"10.21203/rs.3.rs-8742433/v1\",\"editorialEvents\":[],\"status\":\"published\",\"journal\":{\"display\":true,\"email\":\"info@researchsquare.com\",\"identity\":\"communications-earth-and-environment\",\"isNatureJournal\":true,\"hasQc\":false,\"allowDirectSubmit\":false,\"externalIdentity\":\"commsenv\",\"sideBox\":\"Learn more about [Communications Earth and Environment](https://www.nature.com/commsenv/)\",\"snPcode\":\"\",\"submissionUrl\":\"\",\"title\":\"Communications Earth \\u0026 Environment\",\"twitterHandle\":\"\",\"acdcEnabled\":true,\"dfaEnabled\":true,\"editorialSystem\":\"ejp\",\"reportingPortfolio\":\"Communications Series\",\"inReviewEnabled\":true,\"inReviewRevisionsEnabled\":false}}],\"origin\":\"\",\"ownerIdentity\":\"9894689e-cce1-4b4e-a535-f7f21d565097\",\"owner\":[],\"postedDate\":\"February 5th, 2026\",\"published\":true,\"recentEditorialEvents\":[],\"rejectedJournal\":[],\"revision\":\"\",\"amendment\":\"\",\"status\":\"under-review\",\"subjectAreas\":[{\"id\":62256778,\"name\":\"Earth and environmental sciences/Planetary science/Volcanology\"},{\"id\":62256779,\"name\":\"Earth and environmental sciences/Planetary science/Inner planets\"}],\"tags\":[],\"updatedAt\":\"2026-05-01T01:30:29+00:00\",\"versionOfRecord\":[],\"versionCreatedAt\":\"2026-02-05 11:48:23\",\"video\":\"\",\"vorDoi\":\"\",\"vorDoiUrl\":\"\",\"workflowStages\":[]},\"version\":\"v1\",\"identity\":\"rs-8742433\",\"journalConfig\":\"researchsquare\"},\"__N_SSP\":true},\"page\":\"/article/[identity]/[[...version]]\",\"query\":{\"redirect\":\"/article/rs-8742433\",\"identity\":\"rs-8742433\",\"version\":[\"v1\"]},\"buildId\":\"XKTyCvWXoU3ODBz1xrDgd\",\"isFallback\":false,\"isExperimentalCompile\":false,\"dynamicIds\":[84888],\"gssp\":true,\"scriptLoader\":[]}","source_license":"CC-BY-4.0","license_restricted":false}