{"@context":{"@vocab":"https://cir.nii.ac.jp/schema/1.0/","rdfs":"http://www.w3.org/2000/01/rdf-schema#","dc":"http://purl.org/dc/elements/1.1/","dcterms":"http://purl.org/dc/terms/","foaf":"http://xmlns.com/foaf/0.1/","prism":"http://prismstandard.org/namespaces/basic/2.0/","cinii":"http://ci.nii.ac.jp/ns/1.0/","datacite":"https://schema.datacite.org/meta/kernel-4/","ndl":"http://ndl.go.jp/dcndl/terms/","jpcoar":"https://github.com/JPCOAR/schema/blob/master/2.0/"},"@id":"https://cir.nii.ac.jp/crid/1361699993475119104.json","@type":"Article","productIdentifier":[{"identifier":{"@type":"DOI","@value":"10.1029/2018je005647"}},{"identifier":{"@type":"URI","@value":"https://api.wiley.com/onlinelibrary/tdm/v1/articles/10.1029%2F2018JE005647"}},{"identifier":{"@type":"URI","@value":"https://agupubs.onlinelibrary.wiley.com/doi/pdf/10.1029/2018JE005647"}}],"dc:title":[{"@value":"MGS‐TES Spectra Suggest a Basaltic Component in the Regolith of Phobos"}],"description":[{"type":"abstract","notation":[{"@value":"<jats:title>Abstract</jats:title><jats:p>The origins of the Martian moons Phobos and Deimos have been the subjects of considerable debate. Visible and near‐infrared spectra of these bodies are dark and nearly featureless, with red slopes of varying degrees. These spectra are generally consistent with those of carbonaceous asteroids, leading to the hypothesis that Phobos and Deimos are captured carbonaceous asteroids. The shapes and inclinations of the orbits of Phobos and Deimos present problems for the asteroid capture hypothesis. This had led researchers to suggest that Phobos and Deimos coaccreted with Mars or that they are the result of an impact with Mars or in the Mars vicinity. In this work, we reexamine Mars Global Surveyor Thermal Emission Spectrometer (MGS‐TES) data of Phobos and compare spectra of the Phobos surface to mid‐IR spectra of the ungrouped C2 meteorite Tagish Lake (a suggested analog for D‐class asteroids) and particulate basalt and phyllosilicate samples (mixed with carbon black to reduce their visible albedos) acquired in a simulated airless body environment. We find that Tagish Lake is a poor mid‐IR spectral analog to Phobos and that major spectral features in the Phobos spectrum are best matched by a silicate transparency feature similar to that found for finely particulate basalt. Other features in the spectrum are likely best explained by a phyllosilicate component. We suggest that these results indicate that at a portion of the Phobos surface regolith is derived from the Martian crust.</jats:p>"}]}],"creator":[{"@id":"https://cir.nii.ac.jp/crid/1381699993475118976","@type":"Researcher","foaf:name":[{"@value":"Timothy D. Glotch"}],"jpcoar:affiliationName":[{"@value":"Department of Geological Sciences Stony Brook University  Stony Brook NY USA"}]},{"@id":"https://cir.nii.ac.jp/crid/1381699993475119105","@type":"Researcher","foaf:name":[{"@value":"Christopher S. Edwards"}],"jpcoar:affiliationName":[{"@value":"Northern Arizona University  Flagstaff AZ USA"}]},{"@id":"https://cir.nii.ac.jp/crid/1381699993475119104","@type":"Researcher","foaf:name":[{"@value":"Mehmet Yesiltas"}],"jpcoar:affiliationName":[{"@value":"Kirklareli University  Kirklareli Turkey"}]},{"@id":"https://cir.nii.ac.jp/crid/1381699993475119106","@type":"Researcher","foaf:name":[{"@value":"Katherine A. Shirley"}],"jpcoar:affiliationName":[{"@value":"Department of Geological Sciences Stony Brook University  Stony Brook NY USA"}]},{"@id":"https://cir.nii.ac.jp/crid/1381699993475118977","@type":"Researcher","foaf:name":[{"@value":"Dylan S. McDougall"}],"jpcoar:affiliationName":[{"@value":"Department of Geological Sciences Stony Brook University  Stony Brook NY USA"}]},{"@id":"https://cir.nii.ac.jp/crid/1381699993475118979","@type":"Researcher","foaf:name":[{"@value":"Alexander M. Kling"}],"jpcoar:affiliationName":[{"@value":"Department of Geological Sciences Stony Brook University  Stony Brook NY USA"}]},{"@id":"https://cir.nii.ac.jp/crid/1381699993475119107","@type":"Researcher","foaf:name":[{"@value":"Joshua L. Bandfield"}],"jpcoar:affiliationName":[{"@value":"Space Science Institute  Boise ID USA"}]},{"@id":"https://cir.nii.ac.jp/crid/1381699993475118978","@type":"Researcher","foaf:name":[{"@value":"Christopher D. K. Herd"}],"jpcoar:affiliationName":[{"@value":"University of Alberta  Edmonton Alberta Canada"}]}],"publication":{"publicationIdentifier":[{"@type":"PISSN","@value":"21699097"},{"@type":"EISSN","@value":"21699100"}],"prism:publicationName":[{"@value":"Journal of Geophysical Research: Planets"}],"dc:publisher":[{"@value":"American Geophysical Union (AGU)"}],"prism:publicationDate":"2018-10","prism:volume":"123","prism:number":"10","prism:startingPage":"2467","prism:endingPage":"2484"},"reviewed":"false","dc:rights":["http://creativecommons.org/licenses/by-nc-nd/4.0/"],"url":[{"@id":"https://api.wiley.com/onlinelibrary/tdm/v1/articles/10.1029%2F2018JE005647"},{"@id":"https://agupubs.onlinelibrary.wiley.com/doi/pdf/10.1029/2018JE005647"}],"createdAt":"2018-09-24","modifiedAt":"2023-09-15","relatedProduct":[{"@id":"https://cir.nii.ac.jp/crid/1360025430663416064","@type":"Article","resourceType":"学術雑誌論文(journal article)","relationType":["isReferencedBy"],"jpcoar:relatedTitle":[{"@value":"Insights into the origins of Phobos and Deimos based on a spectral comparison with small bodies and Martian materials"}]},{"@id":"https://cir.nii.ac.jp/crid/1360306906082988288","@type":"Article","resourceType":"学術雑誌論文(journal article)","relationType":["isReferencedBy"],"jpcoar:relatedTitle":[{"@value":"Spectro-photometry of Phobos simulants"}]},{"@id":"https://cir.nii.ac.jp/crid/1360865816803777280","@type":"Article","resourceType":"学術雑誌論文(journal article)","relationType":["isReferencedBy"],"jpcoar:relatedTitle":[{"@value":"Origin of Phobos and Deimos Awaiting Direct Exploration"}]},{"@id":"https://cir.nii.ac.jp/crid/1361131420707056512","@type":"Article","resourceType":"学術雑誌論文(journal article)","relationType":["isReferencedBy"],"jpcoar:relatedTitle":[{"@value":"Best practices for the use of meteorite names in publications"}]},{"@id":"https://cir.nii.ac.jp/crid/2051151842060083200","@type":"Article","resourceType":"学術雑誌論文(journal article)","relationType":["isReferencedBy"],"jpcoar:relatedTitle":[{"@value":"Surface environment of Phobos and Phobos simulant UTPS"}]}],"dataSourceIdentifier":[{"@type":"CROSSREF","@value":"10.1029/2018je005647"},{"@type":"CROSSREF","@value":"10.1051/0004-6361/202453080_references_DOI_Rq7kBDJlgc7WnfNlQNrPqXGulKG"},{"@type":"CROSSREF","@value":"10.1016/j.icarus.2024.116216_references_DOI_Rq7kBDJlgc7WnfNlQNrPqXGulKG"},{"@type":"CROSSREF","@value":"10.1186/s40623-021-01406-3_references_DOI_aHg1oq2IYTOBy2gjCEr8O1Z4sIj"},{"@type":"CROSSREF","@value":"10.1146/annurev-earth-040522-110615_references_DOI_Rq7kBDJlgc7WnfNlQNrPqXGulKG"},{"@type":"CROSSREF","@value":"10.1111/maps.13291_references_DOI_Rq7kBDJlgc7WnfNlQNrPqXGulKG"}]}