{"@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/1361418519948560768.json","@type":"Article","productIdentifier":[{"identifier":{"@type":"DOI","@value":"10.1111/maps.12293"}},{"identifier":{"@type":"URI","@value":"https://api.wiley.com/onlinelibrary/tdm/v1/articles/10.1111%2Fmaps.12293"}},{"identifier":{"@type":"URI","@value":"https://onlinelibrary.wiley.com/doi/pdf/10.1111/maps.12293"}}],"dc:title":[{"@value":"The strength of regolith and rubble pile asteroids"}],"description":[{"type":"abstract","notation":[{"@value":"<jats:title>Abstract</jats:title><jats:p>We explore the hypothesis that, due to small van der Waals forces between constituent grains, small rubble pile asteroids have a small but nonzero cohesive strength. The nature of this model predicts that the cohesive strength should be constant independent of asteroid size, which creates a scale dependence with relative strength increasing as size decreases. This model counters classical theory that rubble pile asteroids should behave as scale‐independent cohesionless collections of rocks. We explore a simple model for asteroid strength that is based on these weak forces, validate it through granular mechanics simulations and comparisons with properties of lunar regolith, and then explore its implications and ability to explain and predict observed properties of small asteroids in the <jats:styled-content style=\"fixed-case\">NEA</jats:styled-content> and Main Belt populations, and in particular of asteroid 2008 <jats:styled-content style=\"fixed-case\">TC</jats:styled-content><jats:sub>3</jats:sub>. One conclusion is that the population of rapidly rotating asteroids could consist of both distributions of smaller grains (i.e., rubble piles) and of monolithic boulders.</jats:p>"}]}],"creator":[{"@id":"https://cir.nii.ac.jp/crid/1380013168867327747","@type":"Researcher","foaf:name":[{"@value":"P. Sánchez"}],"jpcoar:affiliationName":[{"@value":"Aerospace Engineering Sciences University of Colorado Boulder Colorado USA"}]},{"@id":"https://cir.nii.ac.jp/crid/1381418519948560768","@type":"Researcher","foaf:name":[{"@value":"D. J. Scheeres"}],"jpcoar:affiliationName":[{"@value":"Engineering Sciences Colorado, The Center for Astrodynamics Research The University of Colorado at Boulder Boulder Colorado USA"}]}],"publication":{"publicationIdentifier":[{"@type":"PISSN","@value":"10869379"},{"@type":"EISSN","@value":"19455100"}],"prism:publicationName":[{"@value":"Meteoritics & Planetary Science"}],"dc:publisher":[{"@value":"Wiley"}],"prism:publicationDate":"2014-05","prism:volume":"49","prism:number":"5","prism:startingPage":"788","prism:endingPage":"811"},"reviewed":"false","dc:rights":["http://onlinelibrary.wiley.com/termsAndConditions#vor"],"url":[{"@id":"https://api.wiley.com/onlinelibrary/tdm/v1/articles/10.1111%2Fmaps.12293"},{"@id":"https://onlinelibrary.wiley.com/doi/pdf/10.1111/maps.12293"}],"createdAt":"2014-05-14","modifiedAt":"2023-10-02","relatedProduct":[{"@id":"https://cir.nii.ac.jp/crid/1050576811657280512","@type":"Article","resourceType":"学術雑誌論文(journal article)","relationType":["isReferencedBy"],"jpcoar:relatedTitle":[{"@language":"en","@value":"Cohesion of regolith: Measurements of meteorite powders"}]},{"@id":"https://cir.nii.ac.jp/crid/1360002215949612288","@type":"Article","resourceType":"学術雑誌論文(journal article)","relationType":["isReferencedBy"],"jpcoar:relatedTitle":[{"@value":"Cratering efficiency on coarse-grain targets: Implications for the dynamical evolution of asteroid 25143 Itokawa"}]},{"@id":"https://cir.nii.ac.jp/crid/1360009142829017600","@type":"Article","resourceType":"学術雑誌論文(journal article)","relationType":["isReferencedBy"],"jpcoar:relatedTitle":[{"@value":"Simulation of Seismic Wave Propagation on Asteroid Ryugu Induced by The Impact Experiment of The Hayabusa2 Mission: Limited Mass Transport by Low Yield Strength of Porous Regolith"}]},{"@id":"https://cir.nii.ac.jp/crid/1360283690926338176","@type":"Article","resourceType":"学術雑誌論文(journal article)","relationType":["isReferencedBy"],"jpcoar:relatedTitle":[{"@value":"Vis-NIR disk-integrated photometry of asteroid 25143 Itokawa around opposition by AMICA/Hayabusa"}]},{"@id":"https://cir.nii.ac.jp/crid/1360286990754069888","@type":"Article","resourceType":"学術雑誌論文(journal article)","relationType":["isReferencedBy"],"jpcoar:relatedTitle":[{"@value":"Small Solar System Bodies as granular media"}]},{"@id":"https://cir.nii.ac.jp/crid/1360298755615664000","@type":"Article","resourceType":"学術雑誌論文(journal article)","relationType":["isReferencedBy"],"jpcoar:relatedTitle":[{"@value":"The ESA Hera Mission: Detailed Characterization of the DART Impact Outcome and of the Binary Asteroid (65803) Didymos"}]},{"@id":"https://cir.nii.ac.jp/crid/1360584341809785344","@type":"Article","resourceType":"学術雑誌論文(journal article)","relationType":["isReferencedBy"],"jpcoar:relatedTitle":[{"@value":"Preliminary design of the Hayabusa2 extended mission to the fast-rotating asteroid 1998 KY26"}]},{"@id":"https://cir.nii.ac.jp/crid/1360857670428071168","@type":"Article","resourceType":"学術雑誌論文(journal article)","relationType":["isReferencedBy"],"jpcoar:relatedTitle":[{"@value":"FOSSIL. II. The Rotation Periods of Small-sized Hilda Asteroids"}]},{"@id":"https://cir.nii.ac.jp/crid/2050307417129956480","@type":"Article","resourceType":"学術雑誌論文(journal article)","relationType":["isReferencedBy"],"jpcoar:relatedTitle":[{"@value":"The MMX rover : performing in situ surface investigations on Phobos"}]}],"dataSourceIdentifier":[{"@type":"CROSSREF","@value":"10.1111/maps.12293"},{"@type":"CROSSREF","@value":"10.1016/j.icarus.2017.09.004_references_DOI_FkwFTKaOpMX7VQTUfhxJ35Kbzch"},{"@type":"CROSSREF","@value":"10.1016/j.icarus.2021.114357_references_DOI_FkwFTKaOpMX7VQTUfhxJ35Kbzch"},{"@type":"CROSSREF","@value":"10.1029/2020je006594_references_DOI_FkwFTKaOpMX7VQTUfhxJ35Kbzch"},{"@type":"CROSSREF","@value":"10.1186/s40623-021-01464-7_references_DOI_FkwFTKaOpMX7VQTUfhxJ35Kbzch"},{"@type":"CROSSREF","@value":"10.1007/s00159-019-0117-5_references_DOI_FkwFTKaOpMX7VQTUfhxJ35Kbzch"},{"@type":"CROSSREF","@value":"10.1016/j.icarus.2018.04.001_references_DOI_FkwFTKaOpMX7VQTUfhxJ35Kbzch"},{"@type":"CROSSREF","@value":"10.3847/psj/ac6f52_references_DOI_FkwFTKaOpMX7VQTUfhxJ35Kbzch"},{"@type":"CROSSREF","@value":"10.1016/j.actaastro.2023.06.010_references_DOI_FkwFTKaOpMX7VQTUfhxJ35Kbzch"},{"@type":"CROSSREF","@value":"10.3847/1538-4365/ac50ac_references_DOI_FkwFTKaOpMX7VQTUfhxJ35Kbzch"}]}