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- W2550331205 abstract "12 Chondritic interplanetary dust particles (IDPs) are subdivided into (1) particles that form highly porous aggregates (chondritic porous ‘CP’ IDPs), and (2) smooth particles (‘CS’ IDPs) [1-3]. Infrared (IR) spectroscopy has been a valuable tool for non-destructively determining the bulk mineralogy of IDPs. Most IDPs fall within three distinct IR groups: (1) olivine-rich particles, (2) pyroxene-rich particles, and (3) phyllosilicate-rich particles [4]. From the IR studies, IDPs dominated by anhydrous minerals tend to be fine grained (CP) [5], while phyllosilicate-rich IDPs are mostly CS [4]. CP IDPs have been linked to cometary sources based on their compositions, spectral properties, and atmospheric entry velocities [6]. Since no spectral signatures of hydrated minerals have been detected in comets, CS IDPs are thought to derive from primitive asteroids [6]. Transmission electron microscopy (TEM) studies have revealed that the mineralogical distinctions between CP and CS IDPs are not always clear. Previous investigators have reported trace amounts of hydrous minerals in dominantly anhydrous particles [7,8]. A better understanding of these particles will help to elucidate whether there is a genetic relationship between anhydrous and hydrated IDPs, provide insight into the earliest stages of aqueous alteration of primitive materials, and may help to determine whether comets have experienced any aqueous processing. Here we report a combined TEM and isotopic imaging study of an unusual anhydrous IDP with hydrated phases." @default.
- W2550331205 created "2016-11-30" @default.
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- W2550331205 date "2005-01-01" @default.
- W2550331205 modified "2023-09-23" @default.
- W2550331205 title "TEM AND NANOSIMS STUDY OF HYDRATED/ ANHYDROUS PHASE MIXED IDPs: COMETARY OR" @default.
- W2550331205 hasPublicationYear "2005" @default.
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