Aqueous Alteration in Hydrated Interplanetary Dust Particles

It is a fundamental goal of interplanetary dust particle (IDP) research to determine the sources and histories of these primitive extraterrestrial materials. Chondritic IDPs have been divided into anhydrous and hydrous varieties, with sub-classification being made on the grounds of the dominant anhydrous (olivine or pyroxene) or hydrous (smectite or serpentine) present. The presumption is that hydrated IDPs experienced aqueous alteration on parent bodies (hydrous asteroids or possibly comets); we wish to discover whether the anhydrous IDPs were the initial raw materials for these reactions. We report here analyses of olivines and pyroxenes from 22 large (>15 um) chondritic IDPs: 18 anhydrous and 4 hydrous; olivines and pyroxenes are scarce in most hydrous IDPs, when present at all Finally, we compare anhydrous to hydrous IDPs, and both to chondritic meteorites.Figure 1 shows our results for this study. We find there to exist no significant difference in the compositions of olivines from olivine vs. pyroxene dominated IDPs, which are therefore plotted together (in contrast to our preliminary results for a smaller data set).

Download Full-text

Cometary dust: the diversity of primitive refractory grains

Philosophical Transactions of The Royal Society A Mathematical Physical and Engineering Sciences ◽

10.1098/rsta.2016.0260 ◽

2017 ◽

Vol 375 (2097) ◽

pp. 20160260 ◽

Cited By ~ 21

Author(s):

D. H. Wooden ◽

H. A. Ishii ◽

M. E. Zolensky

Keyword(s):

Interplanetary Dust ◽

Dust Particles ◽

Refractory Materials ◽

Type Ii ◽

Interplanetary Dust Particles ◽

Aqueous Alteration ◽

Diverse Range ◽

Cometary Dust ◽

Refractory Organic Matter ◽

Comet Dust

Comet dust is primitive and shows significant diversity. Our knowledge of the properties of primitive cometary particles has expanded significantly through microscale investigations of cosmic dust samples (anhydrous interplanetary dust particles (IDPs), chondritic porous (CP) IDPs and UltraCarbonaceous Antarctic micrometeorites, Stardust and Rosetta ), as well as through remote sensing ( Spitzer IR spectroscopy). Comet dust are aggregate particles of materials unequilibrated at submicrometre scales. We discuss the properties and processes experienced by primitive matter in comets. Primitive particles exhibit a diverse range of: structure and typology; distribution of constituents; concentration and form of carbonaceous and refractory organic matter; Mg- and Fe-contents of the silicate minerals; sulfides; existence/abundance of type II chondrule fragments; high-temperature calcium–aluminium inclusions and ameboid-olivine aggregates; and rarely occurring Mg-carbonates and magnetite, whose explanation requires aqueous alteration on parent bodies. The properties of refractory materials imply there were disc processes that resulted in different comets having particular selections of primitive materials. The diversity of primitive particles has implications for the diversity of materials in the protoplanetary disc present at the time and in the region where the comets formed. This article is part of the themed issue ‘Cometary science after Rosetta’.

Download Full-text

Aqueous Alteration in Hydrated Interplanetary Dust Particles

International Astronomical Union Colloquium ◽

10.1017/s0252921100066501 ◽

1991 ◽

Vol 126 ◽

pp. 71-78

Author(s):

Kazushige Tomeoka

Keyword(s):

Significant Proportion ◽

Interplanetary Dust ◽

Chemical Data ◽

Dust Particles ◽

Carbonaceous Chondrites ◽

Interplanetary Dust Particles ◽

Aqueous Alteration ◽

Mineralogical Characteristics ◽

Type Studies ◽

Considerable Detail

AbstractInterplanetary dust particles (IDPs) characterized by chondritic composition can be divided into two principal groups, anhydrous and hydrated. This paper summarizes recent results of mineralogical and petrological studies dealing with the IDPs of hydrated type. Studies on mineralogical characteristics, infrared absorption spectra, and isotopic properties of the hydrated particles have suggested that they are primitive and may contain surviving interstellar material. The hydrated IDPs consist in major part of layer silicates and resemble CI and CM carbonaceous chondrites. Mineralogical and chemical data of both IDPs and carbonaceous chondrites have accumulated, and it is now possible to compare the mineralogies of the IDPs and the meteorites in considerable detail. Evidence was found that a significant proportion of the hydrated IDPs have been processed by aqueous alteration, and the nature of the alteration resembles that of similarly affected meteorites. The mineralogical and chemical data provide important clues to the possible origins of IDPs.

Download Full-text

IDENTIFICATION AND ANALYSIS OF INTERPLANETARY DUST PARTICLES FILTERED FROM ANTARCTIC AIR

10.1130/abs/2018am-321249 ◽

2018 ◽

Author(s):

Katherine Burgess ◽

◽

David Bour ◽

Rhonda M. Stroud ◽

Anais Bardyn ◽

...

Keyword(s):

Interplanetary Dust ◽

Dust Particles ◽

Interplanetary Dust Particles

Download Full-text

On Two Mechanisms of X-Ray Generation in Comets

International Astronomical Union Colloquium ◽

10.1017/s025292110008492x ◽

1985 ◽

Vol 85 ◽

pp. 365-368

Author(s):

S. Ibadov

Keyword(s):

High Temperature ◽

Interplanetary Dust ◽

Dust Particles ◽

Interplanetary Dust Particles ◽

Temperature Plasma ◽

X Ray ◽

Plasma Generation ◽

High Temperature Plasma

AbstractThe intensity of solar X-radiation scattered by a comet is calculated and compared to the proper X-radiation of the comet due to impacts of cometary and interplanetary dust particles. Detection of X-radiation of dusty comets at small heliocentric distances (R ≤ 1 a.u.) is found to be an indicator of high-temperature plasma generation as result of grain collisions.

Download Full-text