Dust impacts at Comet P/Borrelly

Tsurutani, B. T.; Clay, D. R.; Zhang, L. D.; Dasgupta, B.; Brinza, D. E.; Henry, Mike; Mendis, A.; Moses, S. L.; Glaßmeier, Karl‐Heinz; Musmann, G.; Richter, Ingo

doi:10.1029/2003gl017580

Cited by 21 publications

(12 citation statements)

References 15 publications

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“…In this section, we present typical impulsive voltage signals detected by the TDS waveform sampler. As similar voltage pulses have been detected (directly or through their spectral signature) on a number of space missions with various radio and plasma wave instruments in several dusty environments, and were interpreted as dust impacts [ Aubier et al , 1983; Gurnett et al , 1983; Meyer‐Vernet et al , 1986; Oberc , 1990; Tsintikidis et al , 1995; Gurnett et al , 1997; Tsurutani et al , 2003; Kurth et al , 2006], we assume that these pulses are generated by impacts of fast dust particles on the spacecraft. The high sensitivity, time resolution and sampling time of the S/WAVES TDS, as compared to the instruments used in these previous studies, enables us to perform a very careful analysis of these signals at 1 A.U.…”

Section: Dust Impact Detection By S/waves Tdsmentioning

confidence: 99%

Interplanetary dust detection by radio antennas: Mass calibration and fluxes measured by STEREO/WAVES

et al. 2012

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[1] We analyze dust impacts recorded by the S/WAVES radio instrument onboard the two STEREO spacecraft near 1 A.U. during the period 2007-2010. The impact of a dust particle on a spacecraft produces a plasma cloud whose associated electric field can be detected by on-board electric antennas. For this study we use the electric potential time series recorded by the waveform sampler of the instrument. The high time resolution and long sampling times of this measurement enable us to deduce considerably more information than in previous studies based on the dynamic power spectra provided by the same instrument or by radio instruments onboard other spacecraft. The large detection area compared to conventional dust detectors provides flux data with a better statistics. We show that the dust-generated signals are of two kinds, corresponding to impacts of dust from distinctly different mass ranges. We propose calibration formulas for these signals and show that we are able to use S/WAVES as a dust detector with convincing results both in the nanometer and micrometer size ranges. In the latter, the orbital motion of the spacecraft enables us to distinguish between interstellar and interplanetary dust components. Our measurements cover the mass intervals $10 À22 -10 À20 kg and $10 À17 À 5 Â 10 À16 kg. The flux of the larger dust agrees with measurements of other instruments on different spacecraft.

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Section: Dust Impact Detection By S/waves Tdsmentioning

confidence: 99%

Interplanetary dust detection by radio antennas: Mass calibration and fluxes measured by STEREO/WAVES

et al. 2012

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“…The Cassini spacecraft carries the Radio and Plasma Wave Science (RPWS) instrument that, for example, observed the Jovian dust stream particles [ Zook et al , ; Meyer‐Vernet et al , ] and contributed evidence to prove Enceladus as the source of the E ring [ Kurth et al , ]. The Deep Space 1 and Vega spacecraft recorded data in the dust tails of comets Borrelly and Halley [ Oberc et al , ; Oberc and Parzydlo , ; Oberc , ; Tsurutani et al , ; Laakso et al , ]. The STEREO and Wind electric field instruments observed dust impact signatures at 1 AU attributed to interplanetary and interstellar dust [ St Cyr et al , ; Meyer‐Vernet et al , ; Zaslavsky et al , ; Malaspina et al , ].…”

Section: Introductionmentioning

confidence: 99%

Micrometeoroid impact charge yield for common spacecraft materials

et al. 2014

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The impact ionization charge yield is experimentally measured from four common materials used in space and specifically on the two STEREO spacecraft (germanium-coated black Kapton, beryllium copper, multilayer insulation, and solar cells). Cosmic dust particle impacts on spacecraft have been detected by electric field and plasma and radio wave instruments. The accurate interpretation of these signals is complicated by many factors, including the details of the spacecraft antenna system, the local spacecraft plasma environment, and our understanding of the physics of the impact process. The most basic quantity, the amount of charge liberated upon impact, is generally considered poorly constrained and is suspected to depend on the target material. Here we show that for common materials used on spacecraft this variability is small for impacts around 10 km/s, and the impact charge yield can be approximated by 80 fC for a 1 pg projectile. At higher speeds (∼50 km/s), variation of up to a factor of 5 is observed. The measured yields in the 10-50 km/s range are compared to measurements and predictions from the literature and are found to be lower than predicted by at least a factor of 12 at 10 km/s and at least a factor of 1.7 at 50 km/s. Impact charge is also found to depend on angle of incidence; the data suggest a maximum at 45 • .

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“…Dust impacting the spacecraft will influence the plasma environment of the spacecraft and may bias plasma and field measurements. Signals due to impact-generated ion cloudlets have been observed by plasma experiments on several spacecraft in the vicinity of planetary rings (Gurnett et al, 1983;Meyer-Vernet et al, 1986), in the interplanetary medium (Gurnett et al, 1997), and during encounters with the comets Giacobini-Zinner, Halley, and P/Borrelly (Neubauer et al, 1990;Oberc and Parzydlo, 1992;Tsurutani et al, 2003).…”

Section: Solar Probe1 Measurements Of Pickup Ions Created From Materimentioning

confidence: 99%