Abundance, distribution, and origin of 60Fe in the solar protoplanetary disk

By Haolan Tang, N. Dauphas. 2012

181 citations recorded by the source corpus.

Abstract Meteorites contain relict decay products of short-lived radionuclides that were present in the protoplanetary disk when asteroids and planets formed. Several studies reported a high abundance of 60Fe (t1/2=2.62±0.04 Myr) in chondrites (60Fe/56Fe∼6×10−7), suggesting that planetary materials incorporated fresh products of stellar nucleosynthesis ejected by one or several massive stars that exploded in the vicinity of the newborn Sun. We measured 58Fe/54Fe and 60Ni/58Ni isotope ratios in whole rocks and constituents of differentiated achondrites (ureilites, aubrites, HEDs, and angrites), unequilibrated ordinary chondrites Semarkona (LL3.0) and NWA 5717 (ungrouped petrologic type 3.05), metal-rich carbonaceous chondrite Gujba (CBa), and several other meteorites (CV, EL H, LL chondrites; IIIAB, IVA, IVB iron meteorites). We derive from these measurements a much lower initial 60Fe/56Fe ratio of (11.5±2.6)×10−9 and conclude that 60Fe was homogeneously distributed among planetary bodies. This low ratio is consistent with derivation of 60Fe from galactic background (60Fe/56Fe≈2.8×10−7 in the interstellar medium from γ-ray observations) and can be reconciled with high 26Al/27Al∼5×10−5 in chondrites if solar material was contaminated through winds by outer layers of one or several massive stars (e.g., a Wolf–Rayet star) rich in 26Al and poor in 60Fe. We present the first chronological application of the 60Fe–60Ni decay system to establish the time of core formation on Vesta at 3.7 − 1.7 + 2.5  Myr after condensation of calcium–aluminum-rich inclusions (CAIs).

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/831c085139c5b91d25ff60e30dbecae14e94156d

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In Astronomy and Astrophysics

1. N. Dauphas
2. F. Ciesla
3. C. Burkhardt
4. T. Kleine
5. L. Nittler
6. A. Morbidelli
7. Fred C. Adams
8. F. Nimmo

Citations in the corpus

• HETEROGENEOUS DISTRIBUTION OF 26Al AT THE BIRTH OF THE SOLAR SYSTEM (2010, background): “It has been recently inferred that ((60)Fe/(56)Fe)0 in the Solar System is <1 10 8 (Tang and Dauphas, 2012; Wadhwa et al., 2011), much lower than the previous estimates, (5–10) 10 7 (Tachibana et al.”
• The Non-carbonaceous–Carbonaceous Meteorite Dichotomy (2020, background): “…isotope anomalies in CAIs, similar to Cr and Ti, appear to reflect enrichments in the neutron-rich isotopes 62Ni and 64Ni (Birck and Lugmair 1988; Render et al. 2018), those in bulk meteorites largely seem to reflect variations in 58Ni (Nanne et al. 2019; Steele et al. 2012; Tang and Dauphas 2012).”
• Calcium-48 isotopic anomalies in bulk chondrites and achondrites: Evidence for a uniform isotopic reservoir in the inner protoplanetary disk (2014, background): “…groups formed from the same isotopic reservoir (O: Clayton et al., 1984; Ti: Trinquier et al., 2009; Zhang et al., 2012; Cr: Trinquier et al., 2007; Qin et al., 2010; Ni: Steele et al., 2012; Tang and Dauphas, 2012; Regelous et al., 2008; Mo: Dauphas et al., 2002a; Burkhardt et al., 2011).”
• Planetary and meteoritic Mg/Si and δ30Si variations inherited from solar nebula chemistry (2015, background): “, showing that quenched angrites crystallized ~4 Myr after solar system formation while plutonic angrites crystallized ~10 Myr after solar system formation (Kleine et al., 2012; Nyquist et al., 2009; Tang and Dauphas 2012, 2015). As their names indicate, quenched angrites have textures indicative of”
• Astrophysics with Extraterrestrial Materials (2016, background): “…scenarios is hampered both by severe uncertainties in crucial astrophysical aspects, such as nucleosynthetic yields and the details of hydrodynamic mixing of stellar ejecta into cold molecular material, and by changing estimates of SLR abundances in the early Solar System (Tang & Dauphas 2012).”
• EXCLUSION OF COSMIC RAYS IN PROTOPLANETARY DISKS: STELLAR AND MAGNETIC EFFECTS (2013, result): “…was originally attributed to a nearby type II supernova during the formation of the Solar System (Tachibana et al. 2006); however, this result has come under intense scrutiny with later works claiming no such enhancement (Moynier et al. 2011; Dauphas & Chaussidon 2011; Tang & Dauphas 2012).”