Near-earth fragmentation of cosmic dust

Fechtig, H.; Hemenway, C. L.

doi:10.1007/3-540-07615-8_497

Cited by 9 publications

(6 citation statements)

References 6 publications

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“…It is not yet possible to discuss precisely chondritic aggregate history from the total extraterrestrial flux at 1 AU, because an object's mass, density, dynamic strength, composition, and orbital parameters all determine, to a greater or lesser extent, the interpretation of its origins in the interplan- represented in the collected stratospheric dust population nor whether or not these fragments would survive to the collection altitude. Fechtig and Hemenway [1976] have discussed a number of fragmentation mechanisms for micrometeoroid entry and suggested that oxidation fragmentation may be a critical process for low-density, fluffy particles such as CP aggregates (or their precursors). However, the presence of grains in highly reduced states within chondritic aggregates [Fraundorf, 1981] indicates that oxidation fragmentation may not be as significant as originally presumed.…”

Section: A Variety Of Observational Computational and Analytical Mementioning

confidence: 99%

Mineralogy of chondritic interplanetary dust particles

Mackinnon¹,

Rietmeijer²

1987

Reviews of Geophysics

134

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From a mineralogical survey of approximately 30 chondritic micrometeorites collected from the lower stratosphere and studied in detail using current electron microscopy techniques, it is concluded that these particles represent a unique group of extraterrestrial materials. These micrometeorites differ significantly in form and texture from components of carbonaceous chondrites and contain some mineral assemblages which do not occur in any meteorite class. Electron microscope investigations of chondritic micrometeorites have established that these materials (1) are extraterrestrial in origin, (2) existed in space as small objects, (3) endured minimal alteration by planetary processes since formation, and (4) can suffer minimal pulse heating (<600øC) on entering earth's atmosphere. The probable sources for chondritic interplanetary dust particles (IDPs) are cometary and asteroidal debris and, perhaps to a lesser extent, interstellar regions. These sources have not been conclusively linked to any specific mineralogical subset of IDP, although the chondritic porous (CP) aggregate is considered of likely cometary origin. Chondritic IDPs occur in two predominant mineral assemblages:(1) carbonaceous phases and phyllosilicates and (2) carbonaceous phases and nesosilicates or inosilicates, although particles with both types of silicate assemblages are observed. Olivines, pyroxenes, layer silicates, and carbon-rich phases are the most commonly occurring minerals in many chondritic IDPs. Other phases often observed in variable proportions include sulphides, spineIs, metals, metal carbides, carbonates, and minor amounts of sulphates and phosphates. Individual mineral grain sizes range from micrometers (primarily pyroxenes and olivines) to nanometers, with the predominant size for all phases less than 100 nm. Specific mineral characteristics for particular chondritic IDPs provide an indication of processes which may have occurred prior to collection in the earth's stratosphere. For example, pyroxene mineralogy in some chondritic aggregates is consistent with condensation from a vapor phase and, we consider, with condensation in a turbulent solar nebula at relatively low temperatures (<1000øC). Carbonaceous phases present in other CP aggregates have been used to imply low-temperature formation processes such as Fischer-Tropsch synthesis (-530øC) or carbonization and graphitization (--•315øC). Alteration processes have been implicated in the formation of some layer silicates in CP aggregates and may have involved hydrocryogenic alteration at <0øC. In general, interpretations of transformation processes on submicrometer-size minerals in chondritic IDPs are consistent with formation at a radius equivalent to the asteroid belt or greater during the later stages of solar nebula evolution using currently available models.

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Section: A Variety Of Observational Computational and Analytical Mementioning

confidence: 99%

Mineralogy of chondritic interplanetary dust particles

Mackinnon¹,

Rietmeijer²

1987

Reviews of Geophysics

134

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“…These fragmentation effects have been observed by the satellite experiments Prospero (Bedford et al, 1975) and HEOS 2 (Hoffmann et al, 1975b). In a separate paper (Pechtig and Hemenway, 1976) possible fragmentation mechanisms are discussed.…”

Section: Discussion Of Resultsmentioning

confidence: 67%

2.3.3 Micrometeorite Impact Craters on Skylab Experiment S 149

Nagel

Fechtig

Schneider

et al. 1976

International Astronomical Union Colloquium

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During the Skylab experiment S 149 three different sets of areas were exposed. 71-5 cm 2 were facing the sun for 46 days, and 36 cm 2 for 33 days, whereas 77-5 cm 2 were exposed in anti-solar direction for 3^ days. A fourth set is currently being exposed with the hope of future recovery. The exposed surfaces consisted of stainless steel, aluminium, platinum, glass, and pyroxene. The recovered targets have been investigated with a light microscope and a scanning electron microscope. We found two groups of possible impact structures:

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“…Since the GORID sensor has a gathering power of about 15 times that of HEOS-2, it effectively detected a 30 times lower flux of clustered impacts than HEOS-2. 4 If the clusters detected by HEOS-2 and GORID stem for the most part from the same phenomenon (presumably, the magnetospheric swarms), the discrepancy may be explained by the following reasons:…”

Section: (Ii) Geomagnetic Activitymentioning

confidence: 99%

The unresolved mystery of dust particle swarms within the magnetosphere

Sommer

2024

Phil. Trans. R. Soc. A.

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Early-generation in situ dust detectors in near-Earth space have reported the occurrence of clusters of sub-micron dust particles that seemed unrelated to human spaceflight activities. In particular, data from the impact ionization detector onboard the HEOS-2 satellite indicate that such swarms of particles occur throughout the Earth’s magnetosphere up to altitudes of 60 000 km—far beyond regions typically used by spacecraft. Further account of high-altitude clusters has since been given by the GEO-deployed GORID detector, however, explanations for the latter have so far only been sought in GEO spaceflight activity. This perspective piece reviews dust cluster detections in near-Earth space, emphasizing the natural swarm creation mechanism conjectured to explain the HEOS-2 data—i.e. the electrostatic disruption of meteoroids. Highlighting this mechanism offers a novel viewpoint on more recent near-Earth dust measurements. We further show that the impact clusters observed by both HEOS-2 and GORID are correlated with increased geomagnetic activity. This consistent correlation supports the notion that both sets of observations stem from the same underlying phenomenon and aligns with the hypothesis of the electrostatic breakup origin. We conclude that the nature of these peculiar swarms remains highly uncertain, advocating for their concerted investigation by forthcoming dust science endeavours, such as the JAXA/DLR DESTINY + mission. This article is part of the theme issue ‘Dust in the Solar System and beyond’.

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Near-earth fragmentation of cosmic dust

Cited by 9 publications

References 6 publications

Mineralogy of chondritic interplanetary dust particles

Mineralogy of chondritic interplanetary dust particles

2.3.3 Micrometeorite Impact Craters on Skylab Experiment S 149

The unresolved mystery of dust particle swarms within the magnetosphere

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