Hypervelocity dust impacts on the Wind spacecraft: Correlations between Ulysses and Wind interstellar dust detections

Wood, Sandra; Malaspina, D.; Andersson, L.; Horányi, M.

doi:10.1002/2015ja021463

Cited by 23 publications

(23 citation statements)

References 35 publications

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“…These dust observed amplitude and polarity of such signals are consistent with voltage induced on the antennas by positive 290 ions produced by impacts on the spacecraft, after it has recollected the electrons (Meyer-Vernet et al 2014); thisnew mechanism explained the previously unexplained voltage sign and amplitude for interstellar dust impacts on Wind, and also the absence of nanodust detection on this spacecraft. The yearly modulation of Wind-observed impacts was found to be consistent with the yearly variation in interplanetary micron dust, Wood et al 2015. Further supporting this conclusion was the observation that both Wind and STEREO observe 295 the same yearly modulation of interstellar dust flux(Kellogg et al 2016).…”

supporting

confidence: 71%

Dust observations with antenna measurements and its prospects for observations with Parker Solar Probe and Solar Orbiter

Mann¹,

Nouzak²,

Vaverka³

et al. 2019

Preprint

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The electric and magnetic field instrument suite FIELDS on board the NASA Parker Solar Probe and the radio and 15 plasma waves instrument RPWS on the ESA Solar Orbiter mission that explore the inner heliosphere are sensitive to signals generated by dust impacts. Dust impacts were observed using electric field antennas on spacecraft since the 1980s and the method was recently used with a number of space missions to derive dust fluxes. Here, we consider the details of dust impacts, subsequent development of the impact generated plasma and how it produces the measured signals. We describe empirical approaches to characterise the signals and compare to a qualitative discussion of laboratory simulations to predict signal shapes 20 for spacecraft measurements in the inner solar system. While the amount of charge production from a dust impact will be higher near the sun than observed in the interplanetary medium before, the amplitude of pulses will be lower because of the different recovery behaviour that varies with the plasma environment. The photocurrent, that is expected to be higher near the Sun, is found to have moderate influence on the spacecraft potential. 25

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supporting

confidence: 71%

Dust observations with antenna measurements and its prospects for observations with Parker Solar Probe and Solar Orbiter

Mann¹,

Nouzak²,

Vaverka³

et al. 2019

Preprint

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show abstract

“…Discontinuities in the RPWS dust density profile are due to gain changes of WBR. The CDA data showed consistent peak densities of around 0.04 m −3 (threshold ∼ 0.8 µm) during the ringgrazing orbits, less than 1 order of magnitude higher than the RPWS dust density, which is within the uncertainty limit of the method (Ye et al, 2014). The density peak measured by RPWS is wider than that by CDA with a full-width halfmaximum of 600-1000 km compared to 475 km for the latter (averaged profile shows a FWHM of 475 km).…”

Section: Cassinimentioning

confidence: 62%

“…The south-polar plume of Enceladus was one of the top discoveries made by the Cassini mission. During the Enceladus plume crossing, besides dust impact signals, RPWS detected plasma oscillations induced by dust impacts, the frequencies of which are equal to the local plasma frequencies (Ye et al, 2014), which can be explained by a beam-plasma instability induced by the impactproduced electrons when their speed exceeds the thermal speed of the ambient plasma (Meyer-Vernet et al, 2017). Comparison of observations (Ye et al, 2014b) showed that the dust density profile measured by RPWS is consistent with that measured by the dedicated dust detector on board.…”

Section: Cassinimentioning

confidence: 99%

Dust observations with antenna measurements and its prospects for observations with Parker Solar Probe and Solar Orbiter

et al. 2019

View full text Add to dashboard Cite

Abstract. The electric and magnetic field instrument suite FIELDS on board the NASA Parker Solar Probe and the radio and plasma waves instrument RPW on the ESA Solar Orbiter mission that explore the inner heliosphere are sensitive to signals generated by dust impacts. Dust impacts have been observed using electric field antennas on spacecraft since the 1980s and the method was recently used with a number of space missions to derive dust fluxes. Here, we consider the details of dust impacts, subsequent development of the impact generated plasma and how it produces the measured signals. We describe empirical approaches to characterise the signals and compare these in a qualitative discussion of laboratory simulations to predict signal shapes for spacecraft measurements in the inner solar system. While the amount of charge production from a dust impact will be higher near the Sun than observed in the interplanetary medium before, the amplitude of pulses is determined by the recovery behaviour that is different near the Sun since it varies with the plasma environment.

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“…The flux of the larger dust agrees with measurements of other instruments on different spacecraft and one can distinguish in the data between interstellar and interplanetary dust components (Belheouane et al (2012), Zaslavsky et al (2012), Malaspina et al (2015)). The WIND electric field measurements also were analyzed to derive information on hypervelocity dust impacts, the observed flux variation was found to be in good agreement with measurements from dust detectors, while the direction of the interstellar dust flux could not be directly compared and spacecraft orbits are hugely different (Wood et al (2015)). …”

Section: Interstellar and Interplanetary Dust In The Heliospherementioning

confidence: 99%

Division E Commission 49: Interplanetary Plasma and Heliosphere

Mann¹,

Manoharan²,

Gopalswamy³

et al. 2015

Proc. IAU

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Abstract. After a little more than forty years of work related to the interplanetary plasma and the heliosphere the IAU's Commission 49 was formally discontinued in 2015. The commission started its work when the first spacecraft were launched to measure the solar wind in-situ away from Earth orbit, both inward and outward from 1 AU. It now hands over its activities to a new commission during an era of space research when Voyager 1 measures in-situ the parameters of the local interstellar medium at the edge of the heliosphere. The commission will be succeeded by C.E3 with a similar area of responsibility but with more focused specific tasks that the community intends to address during the coming several years. This report includes a short description of the motivation for this commission and of the historical context. It then describes work from 2012 to 2015 during the present solar cycle 24 that has been the weakest in the space era so far. It gave rise to a large number of studies on solar energetic particles and cosmic rays. Other studies addressed e.g. the variation of the solar wind structure and energetic particle fluxes on long time scales, the detection of dust in the solar wind and the Voyager measurements at the edge of the heliosphere. The research is based on measurements from spacecraft that are at present operational and motivated by the upcoming Solar Probe + and Solar Orbiter missions to explore the vicinity of the Sun. We also report here the progress on new and planned radio instruments and their importance for heliospheric studies. Contributors to this report are

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Hypervelocity dust impacts on the Wind spacecraft: Correlations between Ulysses and Wind interstellar dust detections

Cited by 23 publications

References 35 publications

Dust observations with antenna measurements and its prospects for observations with Parker Solar Probe and Solar Orbiter

Dust observations with antenna measurements and its prospects for observations with Parker Solar Probe and Solar Orbiter

Dust observations with antenna measurements and its prospects for observations with Parker Solar Probe and Solar Orbiter

Division E Commission 49: Interplanetary Plasma and Heliosphere

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