Summary of interplanetary and interstellar dust observation by Mars Dust Counter on board NOZOMI

Sasaki, Sho; Igenbergs, E.; Ohashi, Hideo; Senger, R.; Münzenmayer, R.; Naumann, Walter; Grün, E.; Nogami, K.; Mann, I.; Svedhem, H.

doi:10.1016/j.asr.2006.11.006

Cited by 8 publications

(10 citation statements)

References 11 publications

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“…2 ) for about four years in heliocentric distances of 1.0-1.5 AU (Sasaki et al, 2007). ALADDIN's observations exhibited a trend similar to previous observations in which dust flux increased with decreasing distance from the Sun by an approximate factor of 10 (Yano et al, 2011).…”

Section: Introductionsupporting

confidence: 77%

Dust detector using piezoelectric lead zirconate titanate with current-to-voltage converting amplifier for functional advancement

et al. 2013

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This paper describes the concept of a dust monitor using lead zirconate titanate (PZT) ceramics with a large detection area. Its potential as a dust detector is experimentally demonstrated. The dust monitor has a small volume compared to an impact ionization detector with the same detection area, due to the PZT sensor. The PZT sensor, as a traditional device for the in-situ observation of hypervelocity dust particles, has been used for momentum measurement. The hypervelocity impact signals of PZT sensors are typically read by chargesensitive amplifiers. Instead, we suggest a new method that a current-to-voltage converting amplifier is useful for interpreting the impact signal of a PZT sensor arising from dust particles down to 0.5 μm in radius. We propose that datasets of dust impacts can be obtained with a higher statistical accuracy, if the new method is applied to instruments on forthcoming interplanetary-space-cruising spacecrafts.

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Section: Introductionsupporting

confidence: 77%

Dust detector using piezoelectric lead zirconate titanate with current-to-voltage converting amplifier for functional advancement

et al. 2013

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“…The first clear evidence for the detection of LIC grains penetrating into the Solar System was provided by the impact ionization detector on board Ulysses (Grün et al 1994). Subsequently, the identification of LIC grains has been reported by similar detectors on board Hiten, Galileo, and Nozomi, and also confirmed by reanalysis of Helios' data (Svedhem et al 1996;Grün et al 1997;Altobelli et al 2006;Sasaki et al 2007). The Stardust mission has provided a great opportunity to identify the composition of LIC dust by analyzing genuine samples of the dust in the laboratory (Westphal et al 2014b).…”

Section: Introductionmentioning

confidence: 74%

High Radiation Pressure on Interstellar Dust Computed by Light-scattering Simulation on Fluffy Agglomerates of Magnesium-silicate Grains with Metallic-iron Inclusions

Kimura¹

2017

ApJL

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Recent space missions have provided information on the physical and chemical properties of interstellar grains such as the ratio β of radiation pressure to gravity acting on the grains in addition to the composition, structure, and size distribution of the grains. Numerical simulation on the trajectories of interstellar grains captured by Stardust and returned to Earth constrained the β ratio for the Stardust samples of interstellar origin. However, recent accurate calculations of radiation pressure cross-sections for model dust grains have given conflicting stories in the β ratio of interstellar grains. The β ratio for model dust grains of so-called "astronomical silicate" in the femto-kilogram range lies below unity, in conflict with β ∼ 1 for the Stardust interstellar grains. Here, I tackle this conundrum by re-evaluating the β ratio of interstellar grains on the assumption that the grains are aggregated particles grown by coagulation and composed of amorphous MgSiO 3 with the inclusion of metallic iron. My model is entirely consistent with the depletion and the correlation of major rock-forming elements in the Local Interstellar Cloud surrounding the Sun and the mineralogical identification of interstellar grains in the Stardust and Cassini missions. I find that my model dust particles fulfill the constraints on the β ratio derived from not only the Stardust mission but also the Ulysses and Cassini missions. My results suggest that iron is not incorporated into silicates but exists as metal, contrary to the majority of interstellar dust models available to date.

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“…Dust sensors based upon the detection of hyper-velocity impacts were flown on interplanetary space missions such as HEOS and Helios, 9 Pioneer, 5 Nozomi (MDC), 32 Hiten, 33 Giotto (PIA), 34 Ulysses, 35 Galileo, 31,36 Cassini (CDA), 12 Stardust (CIDA), 37 and New Horizon (SDC). 38 Furthermore, the space debris environment was investigated by Debie onboard PROBA (Ref.…”

Section: Applicationsmentioning

confidence: 99%

A 2 MV Van de Graaff accelerator as a tool for planetary and impact physics research

Mocker

Bugiel

Auer³

et al. 2011

Review of Scientific Instruments

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Investigating the dynamical and physical properties of cosmic dust can reveal a great deal of information about both the dust and its many sources. Over recent years, several spacecraft (e.g., Cassini, Stardust, Galileo, and Ulysses) have successfully characterised interstellar, interplanetary, and circumplanetary dust using a variety of techniques, including in situ analyses and sample return. Charge, mass, and velocity measurements of the dust are performed either directly (induced charge signals) or indirectly (mass and velocity from impact ionisation signals or crater morphology) and constrain the dynamical parameters of the dust grains. Dust compositional information may be obtained via either time-of-flight mass spectrometry of the impact plasma or direct sample return. The accurate and reliable interpretation of collected spacecraft data requires a comprehensive programme of terrestrial instrument calibration. This process involves accelerating suitable solar system analogue dust particles to hypervelocity speeds in the laboratory, an activity performed at the Max Planck Institut für Kernphysik in Heidelberg, Germany. Here, a 2 MV Van de Graaff accelerator electrostatically accelerates charged micron and submicron-sized dust particles to speeds up to 80 km s(-1). Recent advances in dust production and processing have allowed solar system analogue dust particles (silicates and other minerals) to be coated with a thin conductive shell, enabling them to be charged and accelerated. Refinements and upgrades to the beam line instrumentation and electronics now allow for the reliable selection of particles at velocities of 1-80 km s(-1) and with diameters of between 0.05 μm and 5 μm. This ability to select particles for subsequent impact studies based on their charges, masses, or velocities is provided by a particle selection unit (PSU). The PSU contains a field programmable gate array, capable of monitoring in real time the particles' speeds and charges, and is controlled remotely by a custom, platform independent, software package. The new control instrumentation and electronics, together with the wide range of accelerable particle types, allow the controlled investigation of hypervelocity impact phenomena across a hitherto unobtainable range of impact parameters.

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Summary of interplanetary and interstellar dust observation by Mars Dust Counter on board NOZOMI

Cited by 8 publications

References 11 publications

Dust detector using piezoelectric lead zirconate titanate with current-to-voltage converting amplifier for functional advancement

Dust detector using piezoelectric lead zirconate titanate with current-to-voltage converting amplifier for functional advancement

High Radiation Pressure on Interstellar Dust Computed by Light-scattering Simulation on Fluffy Agglomerates of Magnesium-silicate Grains with Metallic-iron Inclusions

A 2 MV Van de Graaff accelerator as a tool for planetary and impact physics research

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