Origin of organic matter in the early solar system—VII. The organic polymer in carbonaceous chondrites

1977 ◽  
Vol 41 (9) ◽  
pp. 1325-1339 ◽  
Author(s):  
Ryoichi Hayatsu ◽  
Sumiko Matsuoka ◽  
Robert G. Scott ◽  
Martin H. Studier ◽  
Edward Anders
Keyword(s):  
Organic Matter ◽  
Solar System ◽  
Organic Polymer ◽  
Carbonaceous Chondrites ◽  
Early Solar System

scholarly journals Clues to the early solar system: Extraterrestrial organic molecules in meteorites

2014 ◽  
Vol 36 (6) ◽  
pp. 13-15
Author(s):  
Zita Martins
Keyword(s):  
Organic Matter ◽  
Solar System ◽  
Present Article ◽  
Organic Compounds ◽  
Organic Molecules ◽  
Carbonaceous Chondrites ◽  
Early Solar System ◽  
Very Old ◽  
The Impact

Meteorites are extraterrestrial objects that survive the impact on the Earth's surface. A particular class of meteorites, carbonaceous chondrites, are very old, having remained nearly unaltered since the formation of the solar system approximately 4.6 billion years ago. They contain a rich organic inventory of abiotic molecules with important roles in present day biochemistry. The present article describes the organic compounds present in meteorites, their sources and how to distinguish extraterrestrial organic matter from their terrestrial counterparts.

scholarly journals Investigation of Organic Matter at The Micron Scale in Carbonaceous Chondrites: a Spyglass to Study The Early Solar System.

2016 ◽  
Vol 22 (S3) ◽  
pp. 1788-1789 ◽  
Author(s):  
Laurent Remusat ◽  
Corentin Le Guillou ◽  
Sylvain Bernard ◽  
Vassilissa Vinogradoff ◽  
Adrian Brearley
Keyword(s):  
Organic Matter ◽  
Solar System ◽  
Carbonaceous Chondrites ◽  
Early Solar System

scholarly journals Synthesis of 13C-enriched amino acids with 13C-depleted insoluble organic matter in a formose-type reaction in the early solar system

2021 ◽  
Vol 7 (18) ◽  
pp. eabd3575
Author(s):  
Yoshihiro Furukawa ◽  
Yoshinari Iwasa ◽  
Yoshito Chikaraishi
Keyword(s):  
Aqueous Solution ◽  
Organic Matter ◽  
Solar System ◽  
Acid Synthesis ◽  
Soluble Organic Matter ◽  
Early Solar System ◽  
Cold Region ◽  
Amino Acid Synthesis ◽  
Type Reaction ◽  
Insoluble Organic Matter

Solvent-soluble organic matter (SOM) in meteorites, which includes life’s building molecules, is suspected to originate from the cold region of the early solar system, on the basis of 13C enrichment in the molecules. Here, we demonstrate that the isotopic characteristics are reproducible in amino acid synthesis associated with a formose-type reaction in a heated aqueous solution. Both thermochemically driven formose-type reaction and photochemically driven formose-type reaction likely occurred in asteroids and ice-dust grains in the early solar system. Thus, the present results suggest that the formation of 13C-enriched SOM was not specific to the cold outer protosolar disk or the molecular cloud but occurred more widely in the early solar system.

scholarly journals Oxygen isotopic heterogeneity in the early Solar System inherited from the protosolar molecular cloud

2020 ◽  
Vol 6 (42) ◽  
pp. eaay2724
Author(s):  
Alexander N. Krot ◽  
Kazuhide Nagashima ◽  
James R. Lyons ◽  
Jeong-Eun Lee ◽  
Martin Bizzarro
Keyword(s):  
Solar System ◽  
Molecular Cloud ◽  
Limited Range ◽  
Terrestrial Planets ◽  
Carbonaceous Chondrites ◽  
The Sun ◽  
Early Solar System ◽  
Isotopic Heterogeneity ◽  
Oxygen Isotopic ◽  
O 24

The Sun is 16O-enriched (Δ17O = −28.4 ± 3.6‰) relative to the terrestrial planets, asteroids, and chondrules (−7‰ < Δ17O < 3‰). Ca,Al-rich inclusions (CAIs), the oldest Solar System solids, approach the Sun’s Δ17O. Ultraviolet CO self-shielding resulting in formation of 16O-rich CO and 17,18O-enriched water is the currently favored mechanism invoked to explain the observed range of Δ17O. However, the location of CO self-shielding (molecular cloud or protoplanetary disk) remains unknown. Here we show that CAIs with predominantly low (26Al/27Al)0, <5 × 10−6, exhibit a large inter-CAI range of Δ17O, from −40‰ to −5‰. In contrast, CAIs with the canonical (26Al/27Al)0 of ~5 × 10−5 from unmetamorphosed carbonaceous chondrites have a limited range of Δ17O, −24 ± 2‰. Because CAIs with low (26Al/27Al)0 are thought to have predated the canonical CAIs and formed within first 10,000–20,000 years of the Solar System evolution, these observations suggest oxygen isotopic heterogeneity in the early solar system was inherited from the protosolar molecular cloud.

The thallium isotope composition of carbonaceous chondrites — New evidence for live 205Pb in the early solar system

2010 ◽  
Vol 291 (1-4) ◽  
pp. 39-47 ◽  
Author(s):  
R.G.A. Baker ◽  
M. Schönbächler ◽  
M. Rehkämper ◽  
H.M. Williams ◽  
A.N. Halliday
Keyword(s):  
Solar System ◽  
Isotope Composition ◽  
Carbonaceous Chondrites ◽  
Early Solar System ◽  
New Evidence

Organic matter in carbonaceous meteorites: past, present and future research

2005 ◽  
Vol 363 (1837) ◽  
pp. 2729-2742 ◽  
Author(s):  
Mark A Sephton
Keyword(s):  
Organic Matter ◽  
Solar System ◽  
Chemical Evolution ◽  
Chemical Environment ◽  
Future Research ◽  
Organic Chemical ◽  
Early Solar System ◽  
Organic Mixtures ◽  
Prebiotic Chemical ◽  
Life On Earth

Carbonaceous meteorites are fragments of ancient asteroids that have remained relatively unprocessed since the formation of the Solar System. These carbon-rich objects provide a record of prebiotic chemical evolution and a window on the early Solar System. Many compound classes are present reflecting a rich organic chemical environment during the formation of the planets. Recent theories suggest that similar extraterrestrial organic mixtures may have acted as the starting materials for life on Earth.

scholarly journals Arrival and magnetization of carbonaceous chondrites in the asteroid belt before 4562 million years ago

2020 ◽  
Vol 1 (1) ◽  
Author(s):  
Timothy O’Brien ◽  
John A. Tarduno ◽  
Atma Anand ◽  
Aleksey V. Smirnov ◽  
Eric G. Blackman ◽  
...  
Keyword(s):  
Solar System ◽  
Arrival Time ◽  
Carbonaceous Chondrite ◽  
Parent Body ◽  
Asteroid Belt ◽  
Carbonaceous Chondrites ◽  
Early Solar System ◽  
Outer Disk ◽  
Main Asteroid Belt ◽  
Insight Into

AbstractMeteorite magnetizations can provide rare insight into early Solar System evolution. Such data take on new importance with recognition of the isotopic dichotomy between non-carbonaceous and carbonaceous meteorites, representing distinct inner and outer disk reservoirs, and the likelihood that parent body asteroids were once separated by Jupiter and subsequently mixed. The arrival time of these parent bodies into the main asteroid belt, however, has heretofore been unknown. Herein, we show that weak CV (Vigarano type) and CM (Mighei type) carbonaceous chondrite remanent magnetizations indicate acquisition by the solar wind 4.2 to 4.8 million years after Ca-Al-rich inclusion (CAI) formation at heliocentric distances of ~2–4 AU. These data thus indicate that the CV and CM parent asteroids had arrived near, or within, the orbital range of the present-day asteroid belt from the outer disk isotopic reservoir within the first 5 million years of Solar System history.

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