163 research outputs found
On Presolar Stardust Grains from CO Classical Novae
About 30% to 40% of classical novae produce dust 20-100 days after the
outburst, but no presolar stardust grains from classical novae have been
unambiguously identified yet. Although several studies claimed a nova paternity
for certain grains, the measured and simulated isotopic ratios could only be
reconciled assuming that the grains condensed after the nova ejecta mixed with
a much larger amount of close-to-solar matter. However, the source and
mechanism of this potential post-explosion dilution of the ejecta remains a
mystery. A major problem with previous studies is the small number of
simulations performed and the implied poor exploration of the large nova
parameter space. We report the results of a different strategy, based on a
Monte Carlo technique, that involves the random sampling over the most
important nova model parameters: the white dwarf composition; the mixing of the
outer white dwarf layers with the accreted material before the explosion; the
peak temperature and density; the explosion time scales; and the possible
dilution of the ejecta after the outburst. We discuss and take into account the
systematic uncertainties for both the presolar grain measurements and the
simulation results. Only those simulations that are consistent with all
measured isotopic ratios of a given grain are accepted for further analysis. We
also present the numerical results of the model parameters. We identify 18
presolar grains with measured isotopic signatures consistent with a CO nova
origin, without assuming any dilution of the ejecta. Among these, the grains
G270 2, M11-334-2, G278, M11-347-4, M11-151-4, and Ag2 6 have the highest
probability of a CO nova paternity.Comment: 8 figure
The Effects of Surface Roughness on the NEAR XRS Elemental Results: Monte-Carlo Modeling
The objective of the NEAR-Shoemaker X-ray Gamma-Ray Spec1roscopy ("XGRS") investigation was to determine the elemental composition of the near-Earth asteroid 433 Eros. The X-ray Spectrometer (XRS) system measured the characteristic fluorescence of six major elements (Mg, Al, Si, S, Ca, Fe) in the 1-10 keV energy range excited by the interaction of solar X-rays with the upper 100 microns of the surface of 433 Eros. Various investigators, using both laboratory experiments and computer simulations have established that X-ray fluorescent line ratios can be influenced by small-scale surface roughness at high incidence or emission angles. The effect on the line ratio is specific to the geometry, excitation spectrum, and composition involved, In general, however, the effect is only substantial for ratios of lines with a significant energy difference between them: Fe/Si and Ca/Si are much more likely to be affected than AI/Si or Mg/Si. We apply a Monte-Carlo code to the specific geometry and spectrum of a major NEAR XRS solar flare observation, using an H chondrite composition as the substrate. The seventeen most abundant elements were included in the composition model, from oxygen to titanium
Presolar SIC Grains of Type Y: Origin from Low-Metallicity Asymptotic Giant Branch Stars
We report isotopic data for 27 presolar SiC grains of the rare subtype Y in an acid-resistant residue of the Murchison (CM2) meteorite. Presolar SiC grains of type Y constitute only ~1% of Murchison SiC grains larger than ~2 μm and are defined as having 12C/13C > 100 (solar = 89) and 14N/15N > 272 (solar). In a Si 3-isotope plot, their Si isotopic compositions plot to the right of the correlation line defined by the majority of presolar SiC grains (the mainstream population), whose isotopic compositions indicate an origin in C-rich asymptotic giant branch (AGB) stars of near-solar metallicity. Because of their low abundance, the new Y grains were identified by automatic isotopic imaging of the 12C/13C ratio in the ion microprobe. We report C, N, and Si isotopic ratios of all 27 grains, inferred initial 26Al/27Al ratios of 18, and Ti isotopic ratios of 20 grains. Whereas 14N/15N and 26Al/27Al ratios exhibit the same range as mainstream grains, the C, Si, and Ti isotopic ratios are distinct. Carbon-12/carbon-13 ratios range up to 295 and 30Si/28Si excesses up to 183‰ relative to solar. The average 29Si/28Si ratio of Y grains is by 59‰ smaller than that of mainstream grains. Ti isotopic ratios relative to 48Ti are somewhat similar to those of mainstream grains, but extend to more extreme anomalous compositions. One grain has 46Ti/48Ti, 49Ti/48Ti, and 50Ti/48Ti excesses of 183‰, 365‰, and 990‰, respectively, relative to solar. These features exhibited by Y grains point to an origin in AGB stars of somewhat lower than solar metallicity. In the envelope of such stars the proportion of 12C and s-processed material dredged up from deep zones that experienced partial He burning and was mixed with original material is higher than in stars of solar metallicity. Their envelopes are therefore expected to have larger 12C/13C, 30Si/28Si, and 49Ti/48Ti and 50Ti/48Ti ratios than mainstream grains. We compare the C, Si, and Ti isotopic compositions of Y grains with the results of theoretical models of AGB stars with 1.5, 3, and 5 M☉ and Z = 0.006, 0.01, and 0.02. While solar-metallicity (Z = 0.02) AGB models cannot account for the Y grain data, the models with Z = 0.01 can reproduce the measured isotopic compositions reasonably well. A range of stellar masses (from 1.5 M☉ possibly up to 5 M☉) is indicated by the grain data. The present study together with additional data on SiC grains of type Z furthermore indicate that the rate of change of the ratios of the secondary Si isotopes (29Si and 30Si) relative to 28Si prior to solar system formation was lower than has been generally assumed, implying larger contributions of 28Si from Type Ia supernovae compared to those from Type II supernovae. The Si isotopic ratios of Galactic cosmic rays also suggest such an evolution
On the Mass and Metallicity Distributions of the Parent AGB Stars of O-rich Presolar Stardust Grains
Presolar grains in meteorites formed in a sample of AGB stars that ended
their lives within ~1 Gyr of the origin of the Solar System 4.6 Gyr ago. The
O-isotopic compositions of presolar O-rich stardust reflect the masses and
metallicities of their parent stars. We present simple Monte Carlo simulations
of the parent AGB stars of presolar grains. Comparison of model predictions
with the grain data allow some broad conclusions to be drawn: 1) Presolar
O-rich grains formed in AGB stars of mass ~1.15 - 2.2 MSun. The upper-mass
cutoff reflects dredge-up of C in more massive AGB stars, leading to C-rich
dust rather than O-rich, but the lack of grains from intermediate-mass AGB
stars (>4MSun) is a major puzzle. 2) The grain O-isotopic data are reproduced
well if the Galaxy in presolar times was assumed to have a moderate
age-metallicity relationship, but with significant metallicity scatter for
stars born at the same time. 3) The Sun appears to have a moderately low
metallicity for its age and/or unusual 17O/16O and 18O/16O ratios for its
metallicity. 4) The Solar 17O/18O ratio, while unusual relative to present-day
molecular clouds and protostars, was not atypical for the presolar disk and
does not require self-pollution of the protosolar molecular cloud by supernova
ejecta.Comment: 8 pages, 5 figures; accepted for publication in the Publications of
the Astronomical Society of Australi
Stellar origin of 15N-rich presolar SiC grains of type AB: Supernovae with explosive hydrogen burning
© 2017. The American Astronomical Society. All rights reserved. We report C, N, and Si isotopic data for 59 highly 13 C-enriched presolar submicron-to micron-sized SiC grains from the Murchison meteorite, including eight putative nova grains (PNGs) and 29 15 N-rich ( 14 N/ 15 N ≤ solar) AB grains, and their Mg-Al, S, and Ca-Ti isotope data when available. These 37 grains are enriched in 13 C, 15 N, and 26 Al with the PNGs showing more extreme enhancements. The 15 N-rich AB grains show systematically higher 26 Al and 30 Si excesses than the 14 N-rich AB grains. Thus, we propose to divide the AB grains into groups 1 ( 14 N/ 15 N < solar) and 2 ( 14 N/ 15 N ≥ solar). For the first time, we have obtained both S and Ti isotopic data for five AB1 grains and one PNG and found 32 S and/or 50 Ti enhancements. Interestingly, one AB1 grain had the largest 32 S and 50 Ti excesses, strongly suggesting a neutron-capture nucleosynthetic origin of the 32 S excess and thus the initial presence of radiogenic 32 Si (t 1/2 = 153 years). More importantly, we found that the 15 N and 26 Al excesses of AB1 grains form a trend that extends to the region in the N-Al isotope plot occupied by C2 grains, strongly indicating a common stellar origin for both AB1 and C2 grains. Comparison of supernova models with the AB1 and C2 grain data indicates that these grains came from supernovae that experienced H ingestion into the He/C zones of their progenitors
Automated NanoSIMS Measurements of Spinel Stardust from the Murray Meteorite
We report new O isotopic data on 41 presolar oxide grains, 38 MgAl2O4
(spinel) and 3 Al2O3 from the CM2 meteorite Murray, identified with a recently
developed automated measurement system for the NanoSIMS. We have also obtained
Mg-Al isotopic results on 29 of the same grains (26 spinel and 3 Al2O3). The
majority of the grains have O isotopic compositions typical of most presolar
oxides, fall well into the four previously defined groups, and are most likely
condensates from either red giant branch or asymptotic giant branch stars. We
have also discovered several grains with more unusual O and Mg compositions
suggesting formation in extreme astrophysical environments, such as novae and
supernovae. One of these grains has massive enrichments in 17O, 25Mg, and 26Mg,
which are isotopic signatures indicative of condensation from nova ejecta. Two
grains of supernova origin were also discovered: one has a large 18O/16O ratio
typical of Group 4 presolar oxides; another grain is substantially enriched in
16O, and also contains radiogenic 44Ca from the decay of 44Ti, a likely
condensate from material originating in the O-rich inner zones of a Type II
supernova. In addition, several Group 2 presolar spinel grains also have large
25Mg and 26Mg isotopic anomalies that are difficult to explain by standard
nucleosynthesis in low-mass stars. Auger elemental spectral analyses were
performed on the grains and qualitatively suggest that presolar spinel may not
have higher-than- stoichiometric Al/Mg ratios, in contrast to SIMS results
obtained here and reported previously.Comment: 58 pages, 10 figures, 1 table, published in Ap
New constraints on the major neutron source in low-mass AGB stars
We compare updated Torino postprocessing asymptotic giant branch (AGB)
nucleosynthesis model calculations with isotopic compositions of mainstream SiC
dust grains from low-mass AGB stars. Based on the data-model comparison, we
provide new constraints on the major neutron source, 13C({\alpha},n)16O in the
He-intershell, for the s-process. We show that the literature Ni, Sr, and Ba
grain data can only be consistently explained by the Torino model calculations
that adopt the recently proposed magnetic-buoyancy-induced 13C-pocket. This
observation provides strong support to the suggestion of deep mixing of H into
the He-intershell at low 13C concentrations as a result of efficient transport
of H through magnetic tubes.Comment: ApJ, accepte
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