History of the solar nebula from meteorite paleomagnetism

Weiss, B. P.; Bai, Xue-Ning; Fu, R. R.

doi:10.1126/sciadv.aba5967

Cited by 60 publications

(84 citation statements)

References 211 publications

(330 reference statements)

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“…In this case, taking the 95% confidence lower limits, these data indicate the nebula persisted until >1.22 and >2.51 Ma after CAI formation in these two reservoirs (Table and Figure 7 of Weiss et al. [2021]).…”

Section: Meteorite Paleomagnetismmentioning

confidence: 66%

“…Likewise, paleomagnetic studies of the CV chondrite Kaba, which formed in the carbonaceous reservoir, indicate the field was <0.3 μT by 4.08 ± 0.81 Ma after CAI‐formation (Table and Figure 7 of Weiss et al. [2021]).…”

Section: Meteorite Paleomagnetismmentioning

confidence: 94%

“…This may indicate that the solar nebula persisted until the ∼4–6 Ma formation age of CB chondrules (Bollard et al., 2017; Wölfer et al., 2020) (Table and Table of Weiss et al. [2021]).…”

Section: Meteorite Isotopic Constraints On the Early Growth Of Jupitermentioning

confidence: 99%

“…In particular, it has been found that LL (Fu et al., 2014; Mai et al., 2018) and CM (Cournède et al., 2015) chondrites recorded a midplane field of 54 ± 21 µT and ≳6 µT at 2.03 ± 0.81 Ma and 2.90 ± 0.39 Ma after CAI formation, respectively (Table of Weiss et al. [2021]).…”

Section: Meteorite Paleomagnetismmentioning

confidence: 99%

“…Note that although it was alternatively proposed that CM chondrites were magnetized by the ancient solar wind after the nebula had dispersed (O'Brien et al., 2020), this is unlikely because even if the nebula had cleared by the time CMs were magnetized, the time‐averaged solar wind field at 2 AU was likely >2 orders of magnitude too weak to explain the minimum CM paleointensities (Oran et al., 2018). Furthermore, at the inferred 2.90 ± 0.39 Ma magnetization time of CM chondrites, the nebula was likely still present and would have shielded them against the solar wind (Weiss et al., 2021).…”

Section: Meteorite Paleomagnetismmentioning

confidence: 99%

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What Can Meteorites Tell Us About the Formation of Jupiter?

Weiss

Bottke

2021

AGU Advances

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Gas giants like Jupiter are a fundamental component of planetary systems, but how they formed has been uncertain. Here we discuss how paleomagnetic records in meteorites of the solar nebula may tell us about Jupiter's final growth stage. We suggest that under certain testable assumptions, the meteorite data indicate that proto‐Jupiter grew from a mass of ∼50 Earth masses (M⨁) at >3.46 million years (Ma) after solar system formation to its final mass of 318 M⊕ over just <0.5 Ma. This rapid acceleration is consistent with a key prediction of the core accretion model for giant planet formation.

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Section: Meteorite Paleomagnetismmentioning

confidence: 66%

Section: Meteorite Paleomagnetismmentioning

confidence: 94%

Section: Meteorite Isotopic Constraints On the Early Growth Of Jupitermentioning

confidence: 99%

Section: Meteorite Paleomagnetismmentioning

confidence: 99%

Section: Meteorite Paleomagnetismmentioning

confidence: 99%

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What Can Meteorites Tell Us About the Formation of Jupiter?

Weiss

Bottke

2021

AGU Advances

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Size Ranges of Magnetic Domain States in Tetrataenite

Mansbach

Shah²,

Williams

et al. 2022

Preprint

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Paleomagnetic studies of meteorites provide unique constraints on the evolution of magnetic fields in the early solar system. These studies rely on the identification of magnetic minerals that can retain stable magnetizations over ≳4.5 billion years (Ga). The ferromagnetic mineral tetrataenite (γ''-Fe 0.5 Ni 0.5 ) is found in iron, stony-iron and chondrite meteorite groups. Nanoscale intergrowths of tetrataenite have been shown to carry records of paleomagnetic fields, although the effect of magnetostatic interactions on their magnetic remanence acquisition remains to be fully understood. Tetrataenite can also occur as isolated, non-interacting, nanoscale grains in many meteorite groups, although the paleomagnetic potential of these grains is particularly poorly understood. Here, we aim to improve our understanding of tetrataenite magnetization to refine our knowledge of existing paleomagnetic analyses and broaden the spectrum of meteorite groups that can be used for future paleomagnetic studies. We present the results of analytical calculations and micromagnetic modeling of isolated tetrataenite grains with various geometries. We find that tetrataenite forms a stable single domain state at grain lengths between 6 and ∼160 nm dependent on its elongation. It also possesses a magnetization resistant to viscous remagnetization over the lifetime of the solar system at 293 K. At larger grain sizes, tetrataenite's lowest energy state is a lamellar two-domain state, stable at Ga-scale timescales. Unlike many other magnetic minerals, tetrataenite does not form a single-vortex domain state due to its large uniaxial anisotropy. Our results show that single domain and two-domain tetrataenite grains carry an extremely stable magnetization and therefore are promising for paleomagnetic studies.Plain Language Summary Meteorites are fragments of small bodies created during the early solar system and therefore hold the key to understanding how planets formed and evolved. One way to further this understanding is by studying the magnetic fields recorded by these rocks. To do so requires the identification of magnetic minerals capable of retaining a record of an ancient field (in the form of a measurable magnetization) over the past 4.5 billion years. One mineral that is a potentially reliable recorder is tetrataenite (ordered Fe-Ni metal), which can be resistant to remagnetization by external fields greater than 1 T. The stability of a grain's magnetization is tied to its shape and size. Previous studies of magnetic minerals other than tetrataenite have found that the largest and smallest grains of most magnetic minerals are usually poor recorders with intermediate sizes being the most ideal. Here, we present the results of analytical calculations and numerical modeling of tetrataenite grains with various shapes and sizes to determine the conditions under which tetrataenite magnetization is stable over the lifetime of the solar system. We find that tetrataenite occupies a single-domain state (in which all magnetization is uniform t...

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Setting the Stage: Formation and Earliest Evolution of Io

McKinnon

2023

Astrophysics and Space Science Library

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History of the solar nebula from meteorite paleomagnetism

Cited by 60 publications

References 211 publications

What Can Meteorites Tell Us About the Formation of Jupiter?

What Can Meteorites Tell Us About the Formation of Jupiter?

Size Ranges of Magnetic Domain States in Tetrataenite

Setting the Stage: Formation and Earliest Evolution of Io

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