Instrumentation

Auer, S.

doi:10.1007/978-3-642-56428-4_9

Cited by 39 publications

(27 citation statements)

References 77 publications

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“…In space measurements, the (residual) ionisation of the expanding cloudlet is used to detect the grain. This is applied in classical impact ionisation dust detectors (see [5] for a review) Other space instruments have also observed features that were attributed to dust impacts onto spacecraft, i.e. during comet and planetary rings encounters and in the interplanetary medium (see e.g.…”

Section: Dust and Meteoroids Entering Earth Atmospherementioning

confidence: 99%

“…In this way the mass was derived with a factor of 10 uncertainty and the velocity with factor of 2 uncertainty for dust of masses 10 −19 -10 −11 kg. Even though the dust instruments utilize charge measurements, they only in few cases permit deriving information about the dust surface charge (see [5,66,116] and references there). The Ulysses instrument did not measure the velocity vector of the dust particles, but the detector geometry in combination with the information of the orientation of the spinning spacecraft at the time of the impact restricts the orbits of the dust particles that can reach the detector ( Figure 8 on the left).…”

Section: Dust and Meteoroids Entering Earth Atmospherementioning

confidence: 99%

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Dust in the planetary system: Dust interactions in space plasmas of the solar system

Mann¹,

Meyer‐Vernet²,

Czechowski³

2014

Physics Reports

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Cosmic dust particles are small solid objects observed in the solar planetary system and in many astronomical objects like the surrounding of stars, the interstellar and even the intergalactic medium. In the solar system the dust is best observed and most often found within the region of the orbits of terrestrial planets where the dust interactions and dynamics are observed directly from spacecraft. Dust is observed in space near Earth and also enters the atmosphere of the Earth where it takes part in physical and chemical processes. Hence space offers a laboratory to study dust plasma interactions and dust dynamics. A recent example is the observation of nanodust of sizes smaller than 10 nm. We outline the theoretical considerations on which our knowledge of dust electric charges in space plasmas are founded. We discuss the dynamics of the dust particles and show how the small charged particles are accelerated by the solar wind that carries a magnetic field. Finally, as examples for the space observation of cosmic dust interactions, we describe the first detection of fast nanodust in the solar wind near Earth orbit and the first bi-static observations of PMSE, the radar echoes that are observed in the Earth ionosphere in the presence of charged dust.

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Section: Dust and Meteoroids Entering Earth Atmospherementioning

confidence: 99%

Section: Dust and Meteoroids Entering Earth Atmospherementioning

confidence: 99%

Dust in the planetary system: Dust interactions in space plasmas of the solar system

Mann¹,

Meyer‐Vernet²,

Czechowski³

2014

Physics Reports

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“…The charge yield has been characterized in the laboratory over wide ranges of mass and velocity using dust accelerator facilities (e.g., Auer, 2001;Auer & Sitte, 1968;Burchell et al, 1999;Dietzel et al, 1973;Friichtenicht, 1962;Iglseder & Igenbergs, 1987). The charge yield has been characterized in the laboratory over wide ranges of mass and velocity using dust accelerator facilities (e.g., Auer, 2001;Auer & Sitte, 1968;Burchell et al, 1999;Dietzel et al, 1973;Friichtenicht, 1962;Iglseder & Igenbergs, 1987).…”

Section: Introductionmentioning

confidence: 99%

Magnetic Field Effect on Antenna Signals Induced by Dust Particle Impacts

et al. 2020

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The Radio and Plasma Wave Science instrument on Cassini has observed fewer than expected dust particle impacts during the mission's Grand Finale orbits. The relatively strong magnetic field in the close vicinity of the planet has been suggested to affect the intensity of the dust impact generated signals. A laboratory investigation is performed using dust particles accelerated to ≥20 km/s speed impacting onto a previously developed model of the spacecraft and the Radio and Plasma Wave Science antennas. The external magnetic field is generated by two sets of magnetic coils. The recorded antenna waveforms are decomposed into contributions from the electrons and ions of the dust impact generated plasma cloud. A good qualitative understanding of the waveforms is achieved by dividing the electron and ion population into two portions: one that is escaping from the spacecraft and another that is collected by the spacecraft. The experimental results show that the part of the signal corresponding to escaping electrons is affected by the magnetic field and that dust impact signals can be significantly reduced for spacecraft floating potentials close to zero.

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“…These models have been used to suggest qualitative explanations of the production of plasma in events with high impact velocities (>30 km s −1 ). However, quantitative predictions are generally difficult (for a summary see Auer 2001). By applying an electric field within the region of plasma formation the positive and negative components can be separated and analysed for compositional information (Hansen 1968).…”

Section: Introductionmentioning

confidence: 99%

Time of flight mass spectra of ions in plasmas produced by hypervelocity impacts of organic and mineralogical microparticles on a cosmic dust analyser

Goldsworthy

Burchell

Cole

et al. 2003

A&A

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Abstract. The ionic plasma produced by a hypervelocity particle impact can be analysed to determine compositional information for the original particle by using a time-of-flight mass spectrometer. Such methods have been adopted on interplanetary dust detectors to perform in-situ analyses of encountered grains, for example, the Cassini Cosmic Dust Analyser (CDA). In order to more fully understand the data returned by such instruments, it is necessary to study their response to impacts in the laboratory. Accordingly, data are shown here for the mass spectra of ionic plasmas, produced through the acceleration of microparticles via a 2 MV van de Graaff accelerator and their impact on a dimensionally correct CDA model with a rhodium target. The microparticle dusts examined have three different chemical compositions: metal (iron), organic (polypyrrole and polystyrene latex) and mineral (aluminosilicate clay). These microparticles have mean diameters in the range 0.1 to 1.6 µm and their velocities range from 1-50 km s −1 . They thus cover a wide range of compositions, sizes and speeds expected for dust particles encountered by spacecraft in the Solar System. The advent of new low-density, microparticles with highly controllable attributes (composition, size) has enabled a number of new investigations in this area. The key is the use of a conducting polymer, either as the particle itself or as a thin overlayer on organic (or inorganic) core particles. This conductive coating permits efficient electrostatic charging and acceleration. Here, we examine how the projectile's chemical composition influences the ionic plasma produced after the hypervelocity impact. This study thus extends our understanding of impact plasma formation and detection. The ionization yield normalized to particle mass was found to depend on impact speed to the power (3.4 ± 0.1) for iron and (2.9 ± 0.1) for polypyrrole coated polystyrene and aluminosilicate clay. The ioization signal rise time was found to fall for all projectile materials from a few microseconds at low impact speeds (3 km s −1 ) to a few tenths of a microsecond at higher speeds (approximately 16 km s −1 for aluminosilicate particles and approximately 28 km s −1 for iron and polystyrene particles). At speeds greater than these the rise time was a constant few tenths of a microsecond independent of impact speed. The mass resolution of the time of flight spectrometer was found to be non-linear at high masses above 100 amu. It was ∆m/m = 5 for m = 1 amu and 40 for m = 200 amu. However, although at high masses most mass peaks had the resolution quoted, there were also occasional much narrower mass peaks observed, suggesting that at 250 to 280 amu ∆m/m = 80 to 100. The lower resolutions may be due to closely spaced mass peak signals effectively merging into one observed peak due to the (greater but still finite) resolution found for the isolated mass peaks. Complex mass spectra have been reproducibly obtained from a number of different projectiles that display many charged molecular fragm...

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Instrumentation

Cited by 39 publications

References 77 publications

Dust in the planetary system: Dust interactions in space plasmas of the solar system

Dust in the planetary system: Dust interactions in space plasmas of the solar system

Magnetic Field Effect on Antenna Signals Induced by Dust Particle Impacts

Time of flight mass spectra of ions in plasmas produced by hypervelocity impacts of organic and mineralogical microparticles on a cosmic dust analyser

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