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dc.contributor.authorSingh, V.P.
dc.contributor.authorRudraswami, N.G.
dc.date.accessioned2025-07-04
dc.date.accessioned2025-07-04T06:45:23Z
dc.date.available2025-05-26
dc.date.available2025-07-04T06:45:23Z
dc.date.issued2025
dc.identifier.citationProgress in Earth and Planetary Science,vol.12(1);2025;pp 36
dc.identifier.issn2197-4284
dc.identifier.other10.1186/s40645-025-00710-w
dc.identifier.urihttps://doi.org/10.1186/s40645-025-00710-w
dc.identifier.urihttp://drs.nio.res.in/drs/handle/2264/9465
dc.descriptionIF2023= 3.5
dc.description.abstractCosmic dust, the dominant extraterrestrial material entering Earth's atmosphere, undergoes textural transformation during entry. This study investigates the dependence of texture on entry conditions and classifies textures like barred (tabular, platy, and radial) and porphyritic (equant, skeletal, and chain). Texture development hinges on the balance between overheating and undercooling. Particles heated below the liquidus form scoriaceous or equant porphyritic textures. Near-liquidus temperatures yield skeletal morphologies, while exceeding the liquidus by?~?50��C produces chain forms. At?~?100��C above the liquidus, embryo distortion leads to barred textures, whose type depends on undercooling. Further heating produces cryptocrystalline, glass, and CAT (calcium�aluminium�titanium) spherules. Above 2400��C, ablation exceeds 90% and hindering spherule formation. Additionally, comparing chondritic olivine liquidus and micrometeoroid residual melt compositions with particle heating temperatures reveals the degree of overheating and identifies entry conditions favouring specific textures. Particles with a�size�of 400��m and smaller entering at escape velocity with higher zenith angles (65��90� for CI and 80��90� for CV, CM, L, LL, and H precursors) can survive unmelted or form scoriaceous or porphyritic spherules. Barred textures are likely for smaller particles (<?400��m) entering at escape velocity with moderate zenith angles (50��70�). Steeper angles, larger sizes, and higher velocities favour glass formation. This work refines our understanding of entry conditions that shape micrometeorite textures.
dc.languageen
dc.publisherSpringer
dc.relation.isreferencedbySCI
dc.rightsOnly the author version of the copright reserved papers uploaded. Contact drs@nio.org for any complaints regarding copyright violations
dc.titleTextural evolution of S-type micrometeorites
dc.typeJournal Article
dc.affiliation.authorCSIR-National Institute of Oceanography, Dona Paula, Goa, India


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