Carbon, nitrogen, magnesium, silicon, and titanium isotopic compositions of single interstellar silicon carbide grains from the Murchison carbonaceous chondrite

Hoppe, P.; Amari, S.; Zinner, E.; Ireland, Trevor; Lewis, R. S.

doi:10.1086/174458

Cited by 232 publications

(296 citation statements)

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“…A supernova origin for presolar SiC grains with low 12 C/ 13 C ratios has been discussed by and a nova origin by Amari et al (2001a). However, most of the SiC grains with low 12 C/ 13 C ratios are thought to originate from J-type carbon stars (Hoppe et al 1994(Hoppe et al , 1996 or born-again AGB stars (Amari et al 2001b). J-type carbon stars are solar metallicity stars characterized by strong enrichments in 13 C leading to low 12 C/ 13 C ratios (<15) and enrichments in Li.…”

Section: Graphite Grains With Low 12 C/ 13 C Ratiosmentioning

confidence: 99%

Ne ISOTOPES IN INDIVIDUAL PRESOLAR GRAPHITE GRAINS FROM THE MURCHISON METEORITE TOGETHER WITH He, C, O, Mg-Al ISOTOPIC ANALYSES AS TRACERS OF THEIR ORIGINS

Heck

Amari

Hoppe

et al. 2009

ApJ

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Ne isotopes measured in individual presolar graphite grains, solid samples of extinct stars preserved in primitive meteorites, provide information on the type of stellar sources of the grains and on nucleosynthetic mixing and ion-trapping processes which were operating. We present Ne and He isotope analyses of single presolar graphite grains from the KFB1 density fraction extracted from the carbonaceous chondrite Murchison. In addition, we measured isotopes of C, O, and Mg-Al with the NanoSIMS ion microprobe to better constrain the origin of the grains. Eleven out of 51 presolar graphite grains contain nucleosynthetic 22 Ne above our detection limit. This fraction of 22 Ne-rich grains is similar to the one reported by Nichols et al. although we have a lower 22 Ne detection limit. We detected rare He-shell 20 Ne in one 22 Ne-rich grain and obtained the 20 Ne/ 22 Ne ratio (0.03 ± 0.02) of the He-shell of an Asymptotic Giant Branch (AGB) star with 1.5-2 M and subsolar metallicity. We also detected 4 He in this grain, while in the other grains, which originally acquired He, He-loss seems to be significant. We found unequivocal evidence for radiogenic 22 Ne (Ne-R) in another graphite grain, which likely condensed in a core-collapse supernova and which incorporated live radioactive 22 Na (t 1/2 = 2.6 yr). For the other grains, a clear assignment to a stellar source is more difficult to make. Putative stellar sources are supernovae, AGB stars, born-again AGB stars, J-type carbon stars, and CO novae.

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Section: Graphite Grains With Low 12 C/ 13 C Ratiosmentioning

confidence: 99%

Ne ISOTOPES IN INDIVIDUAL PRESOLAR GRAPHITE GRAINS FROM THE MURCHISON METEORITE TOGETHER WITH He, C, O, Mg-Al ISOTOPIC ANALYSES AS TRACERS OF THEIR ORIGINS

Heck

Amari

Hoppe

et al. 2009

ApJ

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“…Theoretical studies have also shown that large ( 0.1 µm) dust grains form in the winds of AGB stars (Winters et al 1997;Yasuda & Kozasa 2012;Ventura et al 2012). There are also pieces of evidence obtained by meteoritic samples that dust species such as SiC thought to originate from AGB stars from isotopic compositions (Hoppe et al 1994;Daulton et al 2003) have large grain sizes (a 0.1 µm), supporting the formation of large grains in AGB stars Hoppe & Zinner 2000).…”

Section: Review Of the Processesmentioning

confidence: 93%

Two-size approximation: a simple way of treating the evolution of grain size distribution in galaxies

Hirashita

2015

Monthly Notices of the Royal Astronomical Society

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Full calculations of the evolution of grain size distribution in galaxies are in general computationally heavy. In this paper, we propose a simple model of dust enrichment in a galaxy with a simplified treatment of grain size distribution by imposing a 'two-size approximation'; that is, all the grain population is represented by small (grain radius a < 0.03 µm) and large (a > 0.03 µm) grains. We include in the model dust supply from stellar ejecta, destruction in supernova shocks, dust growth by accretion, grain growth by coagulation and grain disruption by shattering, considering how these processes work on the small and large grains. We show that this simple framework reproduces the main features found in full calculations of grain size distributions as follows. The dust enrichment starts with the supply of large grains from stars. At a metallicity level referred to as the critical metallicity of accretion, the abundance of the small grains formed by shattering becomes large enough to rapidly increase the grain abundance by accretion. Associated with this epoch, the mass ratio of the small grains to the large grains reaches the maximum. After that, this ratio converges to the value determined by the balance between shattering and coagulation, and the dust-to-metal ratio is determined by the balance between accretion and shock destruction. With a Monte Carlo simulation, we demonstrate that the simplicity of our model has an advantage in predicting statistical properties. We also show some applications for predicting observational dust properties such as extinction curves.

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“…VIII of this review). Similarly, the discovery of 26 Mg abundance anomalies in meteorites Ireland and Compston, 1987;Gallino et al, 1994, Hoppe et al, 1994Russell et al, 1996), and the discovery of 26 Al in the ISM of our galaxy (Mahoney et al, 1984;Share et al, 1985;MacCallum et al, 1987;von Ballmoos et al, 1987, Diehl et al, 1995 have focused a great deal of attention on the MgAl cycle. The reactions in these two cycles have been subjected to careful experimental scrutiny.…”

Section: H Burning In the Nesi Region: Laboratory Studies A Intmentioning

confidence: 95%

Synthesis of the elements in stars: forty years of progress

et al. 1997

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Forty years ago Burbidge, Burbidge, Fowler, and Hoyle combined what we would now call fragmentary evidence from nuclear physics, stellar evolution and the abundances of elements and isotopes in the solar system as well as a few stars into a synthesis of remarkable ingenuity. Their review provided a foundation for forty years of research in all of the aspects of low energy nuclear experiments and theory, stellar modeling over a wide range of mass and composition, and abundance studies of many hundreds of stars, many of which have shown distinct evidence of the processes suggested by B 2 FH. In this review we summarize progress in each of these fields with emphasis on the most recent developments. [S0034-6861(97)

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Carbon, nitrogen, magnesium, silicon, and titanium isotopic compositions of single interstellar silicon carbide grains from the Murchison carbonaceous chondrite

Cited by 232 publications

References 0 publications

Ne ISOTOPES IN INDIVIDUAL PRESOLAR GRAPHITE GRAINS FROM THE MURCHISON METEORITE TOGETHER WITH He, C, O, Mg-Al ISOTOPIC ANALYSES AS TRACERS OF THEIR ORIGINS

Ne ISOTOPES IN INDIVIDUAL PRESOLAR GRAPHITE GRAINS FROM THE MURCHISON METEORITE TOGETHER WITH He, C, O, Mg-Al ISOTOPIC ANALYSES AS TRACERS OF THEIR ORIGINS

Two-size approximation: a simple way of treating the evolution of grain size distribution in galaxies

Synthesis of the elements in stars: forty years of progress

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