Mn–Cr ages and formation conditions of fayalite in CV3 carbonaceous chondrites

Constraints on the accretion ages of chondritic asteroids

Kaori Jogo, Tomoki Nakamura, Motoo Ito, Shigeru Wakita, Mikhail Zolotov, Scott R. Messenger

Research output: Contribution to journalArticle

4 Citations (Scopus)

Abstract

Chondritic planetesimals are among the first planetary bodies that accreted inside and outside water snow line in the protoplanetary disk. CV3 carbonaceous chondrite parent body accreted relatively small amount of water ice, probably near the snow line, and experienced water-assisted metasomatic alteration that resulted in formation of diverse secondary minerals, including fayalite (Fa80–100). Chemical compositions of the CV3 fayalite and its Mn–Cr isotope systematics indicate that it formed at different temperature (10–300 °C) and fluid pressure (3–300 bars) but within a relatively short period of time. Thermal modeling of the CV3 parent body suggests that it accreted ∼3.2–3.3 Ma after CV3 CAIs formation and had a radius of >110–150 km. The inferred formation age of the CV3 parent body is similar to that of the CM2 chondrite parent body that probably accreted beyond the snow line, but appears to have postdated accretion of the CO and ordinary chondrite parent bodies that most likely formed inside the snow line. The inferred differences in the accretion ages of chondrite parent bodies that formed inside and outside snow line are consistent with planetesimal formation by gravitational/streaming instability.

Original languageEnglish (US)
Pages (from-to)58-74
Number of pages17
JournalGeochimica et Cosmochimica Acta
Volume199
DOIs
StatePublished - Feb 15 2017

Fingerprint

Asteroids
fayalite
carbonaceous chondrite
parent body
Snow
asteroid
accretion
snow
planetesimal
Water
chondrite
Computer aided instruction
Ice
Carbon Monoxide
ordinary chondrite
Isotopes
secondary mineral
Minerals
fluid pressure
water

Keywords

  • Age determination
  • Aqueous alteration
  • CV3 carbonaceous chondrites
  • Equilibrium thermodynamics
  • Fayalite
  • Mn–Cr method
  • Thermal modeling

ASJC Scopus subject areas

  • Geochemistry and Petrology

Cite this

Mn–Cr ages and formation conditions of fayalite in CV3 carbonaceous chondrites : Constraints on the accretion ages of chondritic asteroids. / Jogo, Kaori; Nakamura, Tomoki; Ito, Motoo; Wakita, Shigeru; Zolotov, Mikhail; Messenger, Scott R.

In: Geochimica et Cosmochimica Acta, Vol. 199, 15.02.2017, p. 58-74.

Research output: Contribution to journalArticle

@article{a1fc33c888094a3f9bc020c101d230c0,
title = "Mn–Cr ages and formation conditions of fayalite in CV3 carbonaceous chondrites: Constraints on the accretion ages of chondritic asteroids",
abstract = "Chondritic planetesimals are among the first planetary bodies that accreted inside and outside water snow line in the protoplanetary disk. CV3 carbonaceous chondrite parent body accreted relatively small amount of water ice, probably near the snow line, and experienced water-assisted metasomatic alteration that resulted in formation of diverse secondary minerals, including fayalite (Fa80–100). Chemical compositions of the CV3 fayalite and its Mn–Cr isotope systematics indicate that it formed at different temperature (10–300 °C) and fluid pressure (3–300 bars) but within a relatively short period of time. Thermal modeling of the CV3 parent body suggests that it accreted ∼3.2–3.3 Ma after CV3 CAIs formation and had a radius of >110–150 km. The inferred formation age of the CV3 parent body is similar to that of the CM2 chondrite parent body that probably accreted beyond the snow line, but appears to have postdated accretion of the CO and ordinary chondrite parent bodies that most likely formed inside the snow line. The inferred differences in the accretion ages of chondrite parent bodies that formed inside and outside snow line are consistent with planetesimal formation by gravitational/streaming instability.",
keywords = "Age determination, Aqueous alteration, CV3 carbonaceous chondrites, Equilibrium thermodynamics, Fayalite, Mn–Cr method, Thermal modeling",
author = "Kaori Jogo and Tomoki Nakamura and Motoo Ito and Shigeru Wakita and Mikhail Zolotov and Messenger, {Scott R.}",
year = "2017",
month = "2",
day = "15",
doi = "10.1016/j.gca.2016.11.027",
language = "English (US)",
volume = "199",
pages = "58--74",
journal = "Geochmica et Cosmochimica Acta",
issn = "0016-7037",
publisher = "Elsevier Limited",

}

TY - JOUR

T1 - Mn–Cr ages and formation conditions of fayalite in CV3 carbonaceous chondrites

T2 - Constraints on the accretion ages of chondritic asteroids

AU - Jogo, Kaori

AU - Nakamura, Tomoki

AU - Ito, Motoo

AU - Wakita, Shigeru

AU - Zolotov, Mikhail

AU - Messenger, Scott R.

PY - 2017/2/15

Y1 - 2017/2/15

N2 - Chondritic planetesimals are among the first planetary bodies that accreted inside and outside water snow line in the protoplanetary disk. CV3 carbonaceous chondrite parent body accreted relatively small amount of water ice, probably near the snow line, and experienced water-assisted metasomatic alteration that resulted in formation of diverse secondary minerals, including fayalite (Fa80–100). Chemical compositions of the CV3 fayalite and its Mn–Cr isotope systematics indicate that it formed at different temperature (10–300 °C) and fluid pressure (3–300 bars) but within a relatively short period of time. Thermal modeling of the CV3 parent body suggests that it accreted ∼3.2–3.3 Ma after CV3 CAIs formation and had a radius of >110–150 km. The inferred formation age of the CV3 parent body is similar to that of the CM2 chondrite parent body that probably accreted beyond the snow line, but appears to have postdated accretion of the CO and ordinary chondrite parent bodies that most likely formed inside the snow line. The inferred differences in the accretion ages of chondrite parent bodies that formed inside and outside snow line are consistent with planetesimal formation by gravitational/streaming instability.

AB - Chondritic planetesimals are among the first planetary bodies that accreted inside and outside water snow line in the protoplanetary disk. CV3 carbonaceous chondrite parent body accreted relatively small amount of water ice, probably near the snow line, and experienced water-assisted metasomatic alteration that resulted in formation of diverse secondary minerals, including fayalite (Fa80–100). Chemical compositions of the CV3 fayalite and its Mn–Cr isotope systematics indicate that it formed at different temperature (10–300 °C) and fluid pressure (3–300 bars) but within a relatively short period of time. Thermal modeling of the CV3 parent body suggests that it accreted ∼3.2–3.3 Ma after CV3 CAIs formation and had a radius of >110–150 km. The inferred formation age of the CV3 parent body is similar to that of the CM2 chondrite parent body that probably accreted beyond the snow line, but appears to have postdated accretion of the CO and ordinary chondrite parent bodies that most likely formed inside the snow line. The inferred differences in the accretion ages of chondrite parent bodies that formed inside and outside snow line are consistent with planetesimal formation by gravitational/streaming instability.

KW - Age determination

KW - Aqueous alteration

KW - CV3 carbonaceous chondrites

KW - Equilibrium thermodynamics

KW - Fayalite

KW - Mn–Cr method

KW - Thermal modeling

UR - http://www.scopus.com/inward/record.url?scp=85006833179&partnerID=8YFLogxK

UR - http://www.scopus.com/inward/citedby.url?scp=85006833179&partnerID=8YFLogxK

U2 - 10.1016/j.gca.2016.11.027

DO - 10.1016/j.gca.2016.11.027

M3 - Article

VL - 199

SP - 58

EP - 74

JO - Geochmica et Cosmochimica Acta

JF - Geochmica et Cosmochimica Acta

SN - 0016-7037

ER -