scholarly journals Fine-grained volatile components ubiquitous in solar nebula: Corroboration from scoriaceous cosmic spherules

2018 ◽  
Vol 53 (6) ◽  
pp. 1207-1222 ◽  
Author(s):  
N. G. Rudraswami ◽  
D. Fernandes ◽  
A. K. Naik ◽  
M. Shyam Prasad ◽  
S. Taylor
Keyword(s):  
Solar Nebula ◽  
Volatile Components ◽  
Fine Grained ◽  
Cosmic Spherules

Phyllosilicates and other layer-structured materials in stony meteorites

Clay Minerals ◽  
1985 ◽  
Vol 20 (4) ◽  
pp. 415-454 ◽  
Author(s):  
D. J. Barber
Keyword(s):  
Major Part ◽  
Solar Nebula ◽  
Layered Compounds ◽  
Carbonaceous Chondrites ◽  
Aqueous Alteration ◽  
Structured Materials ◽  
Fine Grained ◽  
Current Thinking ◽  
The Matrix ◽  
Detailed Chemical

AbstractCurrent thinking regarding the possible origins and probable evolutionary histories of meteorites is summarized. Selected data concerning the composition, petrology and other characteristics of the CI and CM groups of stony meteorites in which layered minerals principally occur are then presented. Layered compounds, mainly phyllosilicates, are shown to form a major part of the fine-grained matrix of the CI and CM meteorites, which are classified as carbonaceous chondrites. The results of recent investigations of matrix mineralogy are reviewed, with particular emphasis on the findings of electron microscopy. Several forms of Fe-Mg-serpentine have been identified as the principal phyllosilicates. ‘Poorly-characterized phases’ in CM meteorites have proved to be tochilinite and intergrowths of tochilinite with serpentines. The results generally indicate that the phyllosilicates and most other matrix minerals formed by aqueous alteration in the regoliths of the CI and CM parent bodies; but there is isotopic evidence for the incorporation of components and possibly mineral grains which predate the solar nebula. It is concluded that more detailed chemical and mineralogical information about the phyllosilicates and associated minerals will enable useful constraints to be placed on the possible identities of their precursors and the environments in which both they and the matrix minerals formed.

scholarly journals Discovery of fossil asteroidal ice in primitive meteorite Acfer 094

2019 ◽  
Vol 5 (11) ◽  
pp. eaax5078 ◽  
Author(s):  
Megumi Matsumoto ◽  
Akira Tsuchiyama ◽  
Aiko Nakato ◽  
Junya Matsuno ◽  
Akira Miyake ◽  
...  
Keyword(s):  
Solar Nebula ◽  
Carbonaceous Chondrite ◽  
Parent Body ◽  
Carbonaceous Chondrites ◽  
X Ray ◽  
Porous Texture ◽  
Fine Grained ◽  
X Ray Computed ◽  
Source Materials ◽  
Insight Into

Carbonaceous chondrites are meteorites believed to preserve our planet’s source materials, but the precise nature of these materials still remains uncertain. To uncover pristine planetary materials, we performed synchrotron radiation–based x-ray computed nanotomography of a primitive carbonaceous chondrite, Acfer 094, and found ultraporous lithology (UPL) widely distributed in a fine-grained matrix. UPLs are porous aggregates of amorphous and crystalline silicates, Fe─Ni sulfides, and organics. The porous texture must have been formed by removal of ice previously filling pore spaces, suggesting that UPLs represent fossils of primordial ice. The ice-bearing UPLs formed through sintering of fluffy icy dust aggregates around the H2O snow line in the solar nebula and were incorporated into the Acfer 094 parent body, providing new insight into asteroid formation by dust agglomeration.

scholarly journals Images from the surface of asteroid Ryugu show rocks similar to carbonaceous chondrite meteorites

Science ◽  
2019 ◽  
Vol 365 (6455) ◽  
pp. 817-820 ◽  
Author(s):  
R. Jaumann ◽  
N. Schmitz ◽  
T.-M. Ho ◽  
S. E. Schröder ◽  
K. A. Otto ◽  
...  
Keyword(s):  
Solar Nebula ◽  
Carbonaceous Chondrite ◽  
Aqueous Alteration ◽  
Earth Asteroid ◽  
Fine Grained ◽  
Dark Object ◽  
Sharp Edges ◽  
Fine Grained Material ◽  
Asteroid Surface

The near-Earth asteroid (162173) Ryugu is a 900-m-diameter dark object expected to contain primordial material from the solar nebula. The Mobile Asteroid Surface Scout (MASCOT) landed on Ryugu’s surface on 3 October 2018. We present images from the MASCOT camera (MASCam) taken during the descent and while on the surface. The surface is covered by decimeter- to meter-sized rocks, with no deposits of fine-grained material. Rocks appear either bright, with smooth faces and sharp edges, or dark, with a cauliflower-like, crumbly surface. Close-up images of a rock of the latter type reveal a dark matrix with small, bright, spectrally different inclusions, implying that it did not experience extensive aqueous alteration. The inclusions appear similar to those in carbonaceous chondrite meteorites.

scholarly journals The Question of Presolar Components within Interplanetary Dust Particles (IDPs) Collected in the Stratosphere

2002 ◽  
Vol 12 ◽  
pp. 34-37 ◽  
Author(s):  
John P. Bradley
Keyword(s):  
Solar Nebula ◽  
Carbonaceous Material ◽  
Building Blocks ◽  
Interplanetary Dust ◽  
Dust Particles ◽  
Space Observatory ◽  
Interplanetary Dust Particles ◽  
Infrared Space Observatory ◽  
Fine Grained ◽  
Astronomical Dust

AbstractInterplanetary dust particles (IDPs) are from asteroids and comets, and they are the smallest and most fine-grained meteoritic objects available for laboratory investigation. Cometary IDPs are of special significance because they are presently the only samples of comets, and comets are expected to be enriched in preserved solar nebula and presolar components. These components may include not only cosmically rare refractory circumstellar grains(e.g. SiC) that are recovered from meteorites but also cosmically abundant interstellar silicates and carbonaceous grains that were the fundamental building blocks of the Solar System. D/H ratios measured in IDPs are consistent with the survival of interstellar carbonaceous material, and some IDPs contain glassy grains with properties similar to those of interstellar “amorphous silicates”. Submicrometer forsterite and enstatite crystals in IDPs resemble circumstellar silicates detected by the Infrared Space Observatory (ISO). ISO also detected a broad ~ 23 µm feature around several stars, and a similar feature observed in IDP spectra is due to submicrometer FeNi sulfide grains, suggesting that sulfide grains may be a significant constituent of astronomical dust.

scholarly journals What can pre-solar grains tell us about the solar nebula?

2006 ◽  
Vol 2 (14) ◽  
pp. 353-356 ◽  
Author(s):  
Gary R. Huss ◽  
Bruce T. Draine
Keyword(s):  
Solar System ◽  
Solar Nebula ◽  
Interplanetary Dust ◽  
Radiation Environment ◽  
Dust Particles ◽  
Early Solar System ◽  
Interplanetary Dust Particles ◽  
Fine Grained ◽  
Isotopic Compositions ◽  
Relative Abundances

AbstractSeveral types of pre-solar grains, grains that existed prior to solar system formation, have been found in the fine-grained components of primitive meteorites, interplanetary dust particles (IDPs), and comet samples. Known pre-solar components have isotopic compositions that reflect formation from the ejecta of evolved stars. Other pre-solar materials may have isotopic compositions very similar to solar system materials, making their identification as pre-solar grains problematic. Pre-solar materials exhibit a range of chemical and thermal resistance, so their relative abundances can be used to probe the conditions in the solar nebula. Detailed information on the relative abundances of pre-solar and solar-system materials can provide information on the temperatures, radiation environment, and degree of radial mixing in the early solar system.

Fine-Grained Scoriaceous and Unmelted Micrometeorites: Sources and Relationships with Cosmic Spherules

2018 ◽  
Vol 56 (11) ◽  
pp. 1071-1083 ◽  
Author(s):  
D. D. Badyukov ◽  
F. Brandstaetter ◽  
D. Topa
Keyword(s):  
Fine Grained ◽  
Cosmic Spherules

The Infancy of Solar-Type Stars and its Relevance for the Origin of Life

1997 ◽  
Vol 161 ◽  
pp. 267-282 ◽  
Author(s):  
Thierry Montmerle
Keyword(s):  
Main Sequence ◽  
Solar Nebula ◽  
Circumstellar Disks ◽  
T Tauri Stars ◽  
Necessary Condition ◽  
Sequence Evolution ◽  
T Tauri ◽  
Solar Type ◽  
Optical Domain ◽  
The Origin Of Life

AbstractFor life to develop, planets are a necessary condition. Likewise, for planets to form, stars must be surrounded by circumstellar disks, at least some time during their pre-main sequence evolution. Much progress has been made recently in the study of young solar-like stars. In the optical domain, these stars are known as «T Tauri stars». A significant number show IR excess, and other phenomena indirectly suggesting the presence of circumstellar disks. The current wisdom is that there is an evolutionary sequence from protostars to T Tauri stars. This sequence is characterized by the initial presence of disks, with lifetimes ~ 1-10 Myr after the intial collapse of a dense envelope having given birth to a star. While they are present, about 30% of the disks have masses larger than the minimum solar nebula. Their disappearance may correspond to the growth of dust grains, followed by planetesimal and planet formation, but this is not yet demonstrated.

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