Meteoroid Morphology and Densities: Decoding Satellite Impact Data

McDonnell, J. A. M.; Gardner, David J.

doi:10.1006/icar.1998.5912

Cited by 25 publications

(14 citation statements)

References 17 publications

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“…Taking the meteor density to be 3 g/cm 3 , this distribution yields masses between 10 −12 and 10 −6 g. Note that Evans (1966) used δ = 1 g/cm 3 to calculate the mass of the meteors. The range of our results will not change significantly if we use 1 g/cm 3 or other common meteor densities (Whipple 1952, Murrell et al 1980McDonnell et al 1998). …”

Section: Discussionmentioning

confidence: 52%

Micrometeor Observations Using the Arecibo 430 MHz Radar I. Determination of the Ballistic Parameter from Measured Doppler Velocity and Deceleration Results

Janches

Mathews

Meisel

et al. 2000

Icarus

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Section: Discussionmentioning

confidence: 52%

Micrometeor Observations Using the Arecibo 430 MHz Radar I. Determination of the Ballistic Parameter from Measured Doppler Velocity and Deceleration Results

Janches

Mathews

Meisel

et al. 2000

Icarus

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“…Other impact holes are more irregular in shape, like that in Figure 1d. These holes may be generated by particles with diameters much greater than the film thickness and may serve as a record of the particle's shape [McDonnell and Gardner, 1998]. Alternatively, they may be the result of damage to the impact site post impact.…”

Section: Imaging and Analysis Techniquesmentioning

confidence: 99%

Nanometer hypervelocity dust impacts in low Earth orbit

et al. 2007

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[1] A study has been made of 60 nm thick aluminum films which have been exposed to the space environment outside of International Space Station (ISS) between 2002 and 2004. Field emission scanning electron microscopy has been used to provide high-resolution images of impact features less than 100 nm in diameter and of detailed impact morphologies at different spatial scales. Analysis of images reveals the incident directions and diameters of the impacting particles and allows separation of impacts at hypervelocity from those at lower velocities. This allows the separation of different particle populations. We find that most detected particles have been generated locally as the result of secondaries following larger impacts elsewhere on the ISS or as a result of docking maneuvers by the Progress supply module or by other spacecraft. There is also evidence for a population of dust particles incident at hypervelocity and with minimum diameters smaller than 10 nm. This particle flux of the dust particles is consistent with the expected flux of micrometeoroids with mass >10 À18 g at 1 AU and may represent the first measurement of dust particles with such small masses in near-Earth space. Future experiments to measure the flux of nanometer-scale dust particles are proposed, both passive exposure cells for retrieval and also active detectors to provide access to dust/debris populations without the requirement for experiment retrieval.

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“…on the LDEF mission) has been used to characterize the flux of interplanetary micrometeoroids and man-made space debris particles (e.g. Brownlee, 1995, andMcDonnell et al, 1998).…”

Section: Size Distribution Of Meteoroids Obtained By Microcrater Studiesmentioning

confidence: 99%

The Dawn of Dust Astronomy

2019

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We review the development of dust science from the first ground-based astronomical observations of dust in space to compositional analysis of individual dust particles and their source objects. A multitude of observational techniques is available for the scientific study of space dust: from meteors and interplanetary dust particles collected in the upper atmosphere to dust analyzed in situ or returned to Earth. In situ dust detectors have been developed from simple dust impact detectors determining the dust hazard in Earth orbit to dust telescopes capable of providing compositional analysis and accurate trajectory determination of individual dust particles in space. The concept of Dust Astronomy has been developed, recognizing that dust particles, like photons, carry information from remote sites in space and time. From knowledge of the dust particles' birthplace and their bulk properties, we learn about the remote environment out of which the particles were formed. Dust Observatory missions like Cassini, Stardust, and Rosetta study Saturn's satellites and rings and the dust environments of comet Wild 2 and comet Churyumov-Gerasimenko, respectively. Supplemented by simulations of dusty processes in the laboratory we are beginning to understand the dusty environments in space.

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Meteoroid Morphology and Densities: Decoding Satellite Impact Data

Cited by 25 publications

References 17 publications

Micrometeor Observations Using the Arecibo 430 MHz Radar I. Determination of the Ballistic Parameter from Measured Doppler Velocity and Deceleration Results

Micrometeor Observations Using the Arecibo 430 MHz Radar I. Determination of the Ballistic Parameter from Measured Doppler Velocity and Deceleration Results

Nanometer hypervelocity dust impacts in low Earth orbit

The Dawn of Dust Astronomy

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