Paleomagnetic evidence for a disk substructure in the early solar system

Borlina, C. S.; Weiss, B. P.; Bryson, Joanna J.; Bai, Xue-Ning; Lima, Eduardo A.; Chatterjee, Nilanjan; Mansbach, Elias N.

doi:10.1126/sciadv.abj6928

Cited by 31 publications

(68 citation statements)

References 63 publications

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“…Fig. 7 shows the results of the CO chondrites in context with those of previous studies (Biersteker et al, 2019;Borlina et al, 2021;Bryson et al, 2017Bryson et al, , 2020Cournede et al, 2015;Fu et al, 2014Fu et al, , 2020Fu et al, , 2021Gattacceca et al, 2016;Wang et al, 2017;Weiss et al, 2017). We present in Fig.…”

Section: Solar Nebular Magnetic Fields and Implications For The Dissi...supporting

confidence: 58%

“…(B) Points show paleomagnetic constraints from (A) as a function of age (see text for details on the estimates of the ages). tween 10 −8 and 10 −7 M year −1 and provide lower limits to the accretion rate when compared to that reported by Borlina et al (2021) from dusty olivine chondrules in CO chondrites. Comparing the accretion rate inferred from the lower limit of the paleointensity from the LL chondrules (Fu et al, 2014) to the models shown in Fig.…”

Section: Predicted Midplane Fieldmentioning

confidence: 49%

“…Previous measurements support the presence of nebular fields in the early solar system (Borlina et al, 2021;Cournede et al, 2015;Fu et al, 2021Fu et al, , 2014. The youngest record of the solar nebula in the inner solar system comes from LL chondrules at 2.03 ± 0.81 Myr after CAI formation (Fu et al, 2014;, and the youngest record in the outer solar system comes from the CM chondrites at 3.9 +0.4 −0.5 Myr after CAI formation (Cournede et al, 2015;Fujiya et al, 2012).…”

Section: Solar Nebular Magnetic Fields and Implications For The Dissi...mentioning

confidence: 69%

“…As such, this measured age is likely a proxy for the youngest possible age of magnetite formation on the CO chondrite parent body. Furthermore, Al‐Mg ages of chondrules from CO chondrites suggest that they formed at 2.1 ± 0.8 Myr after CAI‐formation (Borlina et al., 2021; Kita & Ushikubo, 2011) and recent modeling to explain the inventory of CAIs among different chondrite groups suggests that the CO chondrite parent body accreted at ∼2.7 Myr after CAI‐formation (Desch et al., 2018). Thus, we can place a lower limit on the alteration age of the CO chondrites of 2.7 Myr after CAI‐formation, while an upper limit can be obtained by using MAC 88107's alteration age of 5.1 Myr after CAI‐formation.…”

Section: Methodsmentioning

confidence: 99%

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Lifetime of the Outer Solar System Nebula From Carbonaceous Chondrites

et al. 2022

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The lifetimes of protoplanetary disks (PPDs) have important implications for the formation of planetary systems that emerge from them. Determining the lifetime of PPDs (i.e., the dissipation of the gas) constrains the formation time of gas giants and when gas-driven planetary migration can occur. The lifetimes of PPDs have been measured astronomically through observations of dust infrared spectral energy distributions (SEDs) (Haisch et al., 2001;Hernández et al., 2007). SED observations have provided evidence that disks pass through different stages during their evolution from that of protostars to transition disks (disks that have low or no near-infrared excess and high mid-to far-infrared excess) and to debris disks (no remaining gas) (Ercolano & Pascucci, 2017;Owen, 2016). With the exception of a few observed PPDs that are likely in the transition phase, the majority (∼90%) of observed PPDs are either in the PPD phase with a protostar or completely dissipated (Owen, 2016). This observation has been interpreted to suggest that PPDs have a two time-scale evolution during their lifetime: during

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Section: Solar Nebular Magnetic Fields and Implications For The Dissi...supporting

confidence: 58%

Section: Predicted Midplane Fieldmentioning

confidence: 49%

Section: Solar Nebular Magnetic Fields and Implications For The Dissi...mentioning

confidence: 69%

Section: Methodsmentioning

confidence: 99%

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Lifetime of the Outer Solar System Nebula From Carbonaceous Chondrites

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“… 2021 ; Borlina et al. 2021 ). Recent magnetohydrodynamic simulations indicate this field could have been temporally steady for (Weiss et al.…”

Section: How We Will Use Our Data To Determine Psyche’s Originmentioning

confidence: 99%

Distinguishing the Origin of Asteroid (16) Psyche

et al. 2022

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The asteroid (16) Psyche may be the metal-rich remnant of a differentiated planetesimal, or it may be a highly reduced, metal-rich asteroidal material that never differentiated. The NASA Psyche mission aims to determine Psyche’s provenance. Here we describe the possible solar system regions of origin for Psyche, prior to its likely implantation into the asteroid belt, the physical and chemical processes that can enrich metal in an asteroid, and possible meteoritic analogs. The spacecraft payload is designed to be able to discriminate among possible formation theories. The project will determine Psyche’s origin and formation by measuring any strong remanent magnetic fields, which would imply it was the core of a differentiated body; the scale of metal to silicate mixing will be determined by both the neutron spectrometers and the filtered images; the degree of disruption between metal and rock may be determined by the correlation of gravity with composition; some mineralogy (e.g., modeled silicate/metal ratio, and inferred existence of low-calcium pyroxene or olivine, for example) will be detected using filtered images; and the nickel content of Psyche’s metal phase will be measured using the GRNS.

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Size Ranges of Magnetic Domain States in Tetrataenite

Mansbach

Shah²,

Williams

et al. 2022

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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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Paleomagnetic evidence for a disk substructure in the early solar system

Cited by 31 publications

References 63 publications

Lifetime of the Outer Solar System Nebula From Carbonaceous Chondrites

Lifetime of the Outer Solar System Nebula From Carbonaceous Chondrites

Distinguishing the Origin of Asteroid (16) Psyche

Size Ranges of Magnetic Domain States in Tetrataenite

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