Melt migration in rubble-pile planetesimals: Implications for the formation of primitive achondrites

Zhang, Zhongtian; Bercovici, David; Elkins‐Tanton, L. T.

doi:10.1016/j.epsl.2023.118019

Cited by 4 publications

(2 citation statements)

References 71 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“… 81 There are even some more recent results of experiments in low-degree (<15%) partial melts rich in SiO 2 , Al 2 O 3 , and alkali elements that suggest the possibility of widespread high-viscosity silica-rich melts in small bodies of the early Solar System but that the evidence was erased by subsequent stages of melting, accretion, and differentiation. 82 “Primitive achondrites may record melt migration in rubble-pile bodies reaccreted from fragments of partially molten planetesimals.” 83 Thus, it is very likely that some asteroids were more chemically modified respect to others with chondrites generally less differentiated than achondrites. 57 …”

Section: Igneous Processes In Asteroidsmentioning

confidence: 99%

Igneous processes in the small bodies of the Solar System I. Asteroids and comets

Leone¹,

Tanaka²

2023

iScience

View full text Add to dashboard Cite

Section: Igneous Processes In Asteroidsmentioning

confidence: 99%

Igneous processes in the small bodies of the Solar System I. Asteroids and comets

Leone¹,

Tanaka²

2023

iScience

View full text Add to dashboard Cite

“…In these bodies, gas transport would occur first inside the boulders through micropores (i.e., pores between dust grains) toward macropores (i.e., pores between the boulders), and then through macropores toward the surface. Provided that "permeability" is proportional to the square of the characteristic pore size (e.g., Dullien 1992), the effective permeability of a boulder aggregate would be high (as suggested by previous research on melt migration in rubble-pile planetesimals; Zhang et al 2023). Here, we investigate vapor loss from planetesimals that consist of boulders (which themselves are aggregates of fine dust grains) inside the outward-migrating snowline.…”

Section: Introductionmentioning

confidence: 99%

Ice Sublimation in Planetesimals Formed at the Outward Migrating Snowline

Zhang

2023

ApJL

Self Cite

View full text Add to dashboard Cite

Isotopic studies of meteorites suggest that planetesimals were formed as two distinct populations: noncarbonaceous (NC) and carbonaceous (CC) reservoirs. A recent model explains this dichotomy by considering planetesimal formation at the snowline during its migration in the protoplanetary disk, suggesting that NC planetesimals were formed during the outward migration and CC planetesimals were formed during the inward migration. This model has been suggested to contradict meteorite observations because planetesimals formed at the snowline are expected to be rich in H2O and, therefore, develop more oxidizing environments than those inferred from NC iron meteorites. However, if the accreted ice sublimates into vapor without transitioning into a liquid state, the planetesimals may lose most water without being oxidized because reactions between vapor and solids are negligibly slow at temperatures relevant to direct ice sublimation. Here, we investigate the transport of vapor inside a planetesimal and suggest that the pore pressure would have been sufficiently low for direct ice sublimation if (1) the planetesimals were formed during the outward snowline migration (such that they lay inside the snowline after formation and had surfaces permeable to water vapor), (2) these planetesimals were formed by dust-aggregate boulders through “streaming instabilities” instead of being formed directly by submicrometer dust grains, and (3) the boulders were between a few centimeters to ~10 m in size. With these results, the snowline model for NC/CC planetesimal formation may be reconciled with the observations of iron meteorite oxidation states.

show abstract

Trace elements in IVA iron meteorites explained by limited solid–liquid equilibration during inward solidification

Zhang

2024

Icarus

View full text Add to dashboard Cite

Melt migration in rubble-pile planetesimals: Implications for the formation of primitive achondrites

Cited by 4 publications

References 71 publications

Igneous processes in the small bodies of the Solar System I. Asteroids and comets

Igneous processes in the small bodies of the Solar System I. Asteroids and comets

Ice Sublimation in Planetesimals Formed at the Outward Migrating Snowline

Trace elements in IVA iron meteorites explained by limited solid–liquid equilibration during inward solidification

Contact Info

Product

Resources

About