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• W2000224549 startingPage "10363" @default.
• W2000224549 abstract "Some portion of the interstellar dust entering the heliosphere is a refractory (Ca‐Al‐Ti‐Mg‐Si‐Fe‐Ni‐Cr‐Co‐rich) component either condensed at high temperature from stellar outflows or formed in the interstellar medium (ISM). Condensation sequences for T >1100 K, assuming chemical equilibrium, are calculated for stellar outflow gas having (1) solar composition at various P tot ; (2) compositions approaching C/O=0.9, otherwise solar; (3) metallicities reduced by Z/Z o =0.10; and (4) metallicities enhanced by added dust components. Calculated depletions are relatively insensitive to these excursions from the canonical “cosmic” abundances. The intragroup similarities of depletions observed for the element groups (Ca‐Ti), (Fe‐Ni‐Cr‐Co), and (Mg‐Si) reflect the dominant mineralogy calculated for Stardust: Ti‐ and Ca‐aluminate phases, metal alloy, and Mg 2 SiO 4 (Mg‐olivine). This result suggests that the bulk of the refractory component of ISM dust was condensed in stellar environments." @default.
• W2000224549 created "2016-06-24" @default.
• W2000224549 creator A5040167717 @default.
• W2000224549 date "2000-05-01" @default.
• W2000224549 modified "2023-09-27" @default.
• W2000224549 title "Variations on solar condensation: Sources of interstellar dust nuclei" @default.
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• W2000224549 doi "https://doi.org/10.1029/1999ja900192" @default.
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