An investigation into the origin of Fe-rich presolar silicates in ACFER 094

Maitrayee Bose, Christine Floss, Frank J. Stadermann

Research output: Contribution to journalArticle

33 Citations (Scopus)

Abstract

Presolar silicate and oxide grains from primitive meteorites are recognized as "stardust" on the basis of their extremely anomalous O isotopic compositions. We report data on 48 O-anomalous grains that were identified in grain size separates of the ungrouped carbonaceous chondrite Acfer 094. A majority of these grains exhibit high 17O/16O isotopic ratios along with solar to sub-solar 18O/16O ratios and may have originated in low-mass stars with close-to-solar metallicity. Four silicate grains that contain 18O enrichments were also measured for their Si isotopes. A comparison of their O and Si isotopic compositions with model predictions indicates that these 18O-rich grains may have formed in supernova ejecta. Four of the O-anomalous grains are oxides while the remaining 44 are silicates, based on elemental compositions determined by Auger spectroscopy. The presolar oxides include a TiO2 grain and a grain with spinel stoichiometry. The silicate grains largely exhibit ferromagnesian compositions, although a few grains also contain small amounts of Ca and/or Al. Stoichiometric silicates were further classified as either olivine-like or pyroxene-like, and in this study pyroxene-like grains are more abundant than olivine-like ones. The majority of silicates contain more Fe than Mg, including a few grains with Fe-rich end-member compositions. Spectroscopic observations indicate the presence of Mg-rich silicates in the atmospheres of stars and the interstellar medium. Mg-rich minerals such as forsterite and enstatite form by equilibrium condensation in stellar environments. However, non-equilibrium condensation can result in higher Fe contents and the occurrence of such processes in the outflows of stars may account for the Fe-rich grains. Alternatively, secondary processes may play a role in producing the Fe enrichments observed in the presolar silicate grains identified in the matrix of Acfer 094.

Original languageEnglish (US)
Pages (from-to)1624-1636
Number of pages13
JournalAstrophysical Journal
Volume714
Issue number2
DOIs
StatePublished - Jan 1 2010
Externally publishedYes

Fingerprint

silicates
silicate
oxide
pyroxene
condensation
olivine
isotopic composition
enstatite
carbonaceous chondrite
forsterite
stars
stoichiometry
oxides
isotopic ratio
ejecta
meteorite
spinel
outflow
grain size
spectroscopy

Keywords

  • Astrochemistry
  • Circumstellar matter
  • Stars: AGB and post-AGB
  • Supernovae: general

ASJC Scopus subject areas

  • Astronomy and Astrophysics
  • Space and Planetary Science

Cite this

An investigation into the origin of Fe-rich presolar silicates in ACFER 094. / Bose, Maitrayee; Floss, Christine; Stadermann, Frank J.

In: Astrophysical Journal, Vol. 714, No. 2, 01.01.2010, p. 1624-1636.

Research output: Contribution to journalArticle

Bose, Maitrayee ; Floss, Christine ; Stadermann, Frank J. / An investigation into the origin of Fe-rich presolar silicates in ACFER 094. In: Astrophysical Journal. 2010 ; Vol. 714, No. 2. pp. 1624-1636.
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AB - Presolar silicate and oxide grains from primitive meteorites are recognized as "stardust" on the basis of their extremely anomalous O isotopic compositions. We report data on 48 O-anomalous grains that were identified in grain size separates of the ungrouped carbonaceous chondrite Acfer 094. A majority of these grains exhibit high 17O/16O isotopic ratios along with solar to sub-solar 18O/16O ratios and may have originated in low-mass stars with close-to-solar metallicity. Four silicate grains that contain 18O enrichments were also measured for their Si isotopes. A comparison of their O and Si isotopic compositions with model predictions indicates that these 18O-rich grains may have formed in supernova ejecta. Four of the O-anomalous grains are oxides while the remaining 44 are silicates, based on elemental compositions determined by Auger spectroscopy. The presolar oxides include a TiO2 grain and a grain with spinel stoichiometry. The silicate grains largely exhibit ferromagnesian compositions, although a few grains also contain small amounts of Ca and/or Al. Stoichiometric silicates were further classified as either olivine-like or pyroxene-like, and in this study pyroxene-like grains are more abundant than olivine-like ones. The majority of silicates contain more Fe than Mg, including a few grains with Fe-rich end-member compositions. Spectroscopic observations indicate the presence of Mg-rich silicates in the atmospheres of stars and the interstellar medium. Mg-rich minerals such as forsterite and enstatite form by equilibrium condensation in stellar environments. However, non-equilibrium condensation can result in higher Fe contents and the occurrence of such processes in the outflows of stars may account for the Fe-rich grains. Alternatively, secondary processes may play a role in producing the Fe enrichments observed in the presolar silicate grains identified in the matrix of Acfer 094.

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