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

Zaslavsky, A.; Meyer‐Vernet, N.; Mann, Ingrid; Czechowski, A.; Issautier, Karine; Chat, Gaétan Le; Pantellini, Filippo; Goetz, K.; Maksimović, M.; Bale, S. D.; Kasper, J. C.

doi:10.1029/2011ja017480

Cited by 103 publications

(267 citation statements)

References 44 publications

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“…The interplanetary dust population along Itokawa's orbital path is probably contained within the two flux curves. The interplanetary dust flux model is in good agreement with dust detections at 1 AU by the Ulysses ( Wehry and Mann, 1999 ) and STEREO spacecraft ( Meyer-Vernet et al, 2009;Zaslavsky et al, 2012 ). Grün et al (1985) also constructed the impact flux curve pertaining to the lunar surface ( Fig.…”

Section: Origin Of Submicrometer Cratersmentioning

confidence: 64%

Population characteristics of submicrometer-sized craters on regolith particles from asteroid Itokawa

Matsumoto

Hasegawa

Nakao

et al. 2018

Icarus

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a b s t r a c tWe investigated impact crater structures on regolith particles from asteroid Itokawa using scanning electron microscopy. We observed the surfaces of 51 Itokawa particles, ranging from 15 μm to 240 μm in size. Craters with average diameters ranging from 10 nm to 2.8 μm were identified on 13 Itokawa particles larger than 80 μm. We examined the abundance, spatial distribution, and morphology of approximately 900 craters on six Itokawa particles. Craters with sizes in excess of 200 nm are widely dispersed, with spatial densities from 2.6 μm 2 to 4.5 μm 2 ; a fraction of the craters was locally concentrated with a density of 0.1 μm 2 . The fractal dimension of the cumulative crater diameters ranges from 1.3 to 2.3. Craters of several tens of nanometers in diameter exhibit pit and surrounding rim structures. Craters of more than 100 nm in diameter commonly have melted residue at their bottom. These morphologies are similar to those of submicrometer-sized craters on lunar regolith. We estimated the impactor flux on Itokawa regolith-forming craters, assuming that the craters were accumulated during direct exposure to the space environment for 10 2 to 10 4 yr. The range of impactor flux onto Itokawa particles is estimated to be at least one order of magnitude higher than the interplanetary dust flux and comparable to the secondary impact flux on the Moon. This indicates that secondary ejecta impacts are probably the dominant cratering process in the submicrometer range on Itokawa regolith particles, as well as on the lunar surface. We demonstrate that secondary submicrometer craters can be produced anywhere in centimeter-to meter-sized depressions on Itokawa's surface through primary interplanetary dust impacts. If the surface unevenness on centimeter to meter scales is a significant factor determining the abundance of submicrometer secondary cratering, the secondary impact flux could be independent of the overall shapes or sizes of celestial bodies, and the secondary impact flux could have similar values on Itokawa and the Moon.

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Section: Origin Of Submicrometer Cratersmentioning

confidence: 64%

Population characteristics of submicrometer-sized craters on regolith particles from asteroid Itokawa

Matsumoto

Hasegawa

Nakao

et al. 2018

Icarus

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“…Nanodust as a component of the solar system dust cloud The flux of nanodust derived from the STEREO measurements is close to the curve obtained from extrapolating the previous observations near 1 AU to smaller sizes as seen in Figure (24), which shows the average fluxes of nanodust derived from the plasma wave measurements [168,166,13,243]. It was mentioned above that the collisional evolution of the dust cloud generates dust over a broad range of sizes described in models of a flux versus mass curve at 1 AU [62,25,94].…”

mentioning

confidence: 69%

“…[70,161,180,182,183,71,223]). Motivated by observations, the physics underlying the dust observations with radio and plasma wave instruments has been discussed (see reviews [184,164]), Observations have been recently refined by using a new generation of high speed radio receivers [243,124]. The instruments typically detect impacts of particles of sizes of several nm and larger.…”

Section: Dust and Meteoroids Entering Earth Atmospherementioning

confidence: 99%

“…Its extrapolation to nanometric sizes is shown in Figure (24) and the indicated flux curve ∼ m −5/6 results from the small bodies fragmentation theory [40] and would be observed in the absence of other effects. Note, that the same instrument also observed the impacts of larger dust particle, including impacts that could be attributed to interstellar dust [13,243].…”

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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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“…The evaluation of nanodust fluxes based on analysis of ongoing measurements with plasma wave instruments onboard the two Stereo spacecraft near 1 AU (Zaslavsky et al, 2012) provide a basis for our estimate. We assume the following typical parameters for nanodust at the orbit of Earth: 10 −22 kg < m d < 10 −20 kg, 3×10 −7 m −3 < N d < 3× 10 −5 m −3 , and Q d = 17e.…”

Section: An Extended Version Of the Treumann And Baumjohann Modelmentioning

confidence: 99%

Dust dynamic pressure and magnetopause displacement: reasons for non-detection

Mann

Hamrin

2013

Ann. Geophys.

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Abstract. In a recent paper, Treumann and Baumjohann (2011) propose that the contribution of dust particles to the solar wind dynamic pressure can cause large compressions of the Earth's magnetopause and suggest that this occurs when Earth encounters meteoroid streams. In this paper we estimate the contribution from charged dust particles to the solar wind dynamical pressure, and we exclude that the dust associated to meteoroid streams can influence the extension of the magnetopause according to the proposed model. A sufficient coupling to the solar wind is only expected for so-called nanodust. However, the dynamic pressure of the nanodust is orders of magnitudes below that of the solar wind, making it unlikely that its variation can be observed in displacements of the magnetopause. We also discuss the equation that the authors use for estimating the extension of the Earth's magnetopause, and conclude that this is not applicable due to the large gyroradius of the nanodust. We finally note that an influence of dust on the extension of a magnetosphere might be quite possible in other astrophysical systems and based on other processes.

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

Cited by 103 publications

References 44 publications

Population characteristics of submicrometer-sized craters on regolith particles from asteroid Itokawa

Population characteristics of submicrometer-sized craters on regolith particles from asteroid Itokawa

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

Dust dynamic pressure and magnetopause displacement: reasons for non-detection

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