Optical and Thermal Properties of Interplanetary Dust

Levasseur-Regourd, A. C.; Mann, Ingrid; Dumont, René; Hanner, M. S.

doi:10.1007/978-3-642-56428-4_2

Cited by 41 publications

(50 citation statements)

References 79 publications

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“…This relation is approximately valid between 1.5 and 0.5 AU as deduced from the infrared observations (Dumont & Levasseur-Regourd 1988;Reach 1991;Renard et al 1995;Levasseur-Regourd et al 2001). …”

Section: Temperaturesupporting

confidence: 59%

“…Levasseur-Regourd et al 2001), and it peaks around 550 nm. As a first approximation, for the calculations of light scattering, the complex index of the particles is taken around this particular wavelength.…”

Section: Optical Constants Of the Particlesmentioning

confidence: 99%

“…Consequently, techniques of inversion, such as the "nodes of lesser uncertainty" method (see e.g. Dumont & Levasseur-Regourd 1988;Levasseur-Regourd et al 2001, and references therein) are needed to retrieve the local properties. All the values given in the following text correspond to bulk values deduced from inversion methods over elementary volumes.…”

Section: Introductionmentioning

confidence: 99%

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Inferring the interplanetary dust properties

Lasue¹,

Levasseur-Regourd²,

Fray

et al. 2007

A&A

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Context. Since in situ studies and interplanetary dust collections only provide a spatially limited amount of information about the interplanetary dust properties, it is of major importance to complete these studies with properties inferred from remote observations of scattered and emitted light, with interpretation through simulations. Aims. Physical properties of the interplanetary dust in the near-ecliptic symmetry surface, such as the local polarization, temperature, and composition, together with their heliocentric variations, may be derived from scattered and emitted light observations, giving clues to the respective contribution of the particle sources. Methods. A model of light scattering by a cloud of solid particles constituted by spheroidal grains and aggregates thereof is used to interpret the local light-scattering data. Equilibrium temperature of the same particles allows us to interpret the temperature heliocentric variations. Results. A good fit of the local polarization phase curve, P α , near 1.5 AU from the Sun is obtained for a mixture of silicates and more absorbing organic material (≈40% in mass) and for a realistic size distribution typical of the interplanetary dust in the 0.2 µm to 200 µm size range. The contribution of dust particles of cometary origin is at least 20% in mass. The same size distribution of particles gives a dependence of the temperature with the solar distance, R, in R −0.45 that is different than the typical black body behavior. The heliocentric dependence of P α=90 • is interpreted as a progressive disappearance of solid organic (such as HCN polymers or amorphous carbon) towards the Sun. Conclusions.

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Section: Temperaturesupporting

confidence: 59%

Section: Optical Constants Of the Particlesmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Inferring the interplanetary dust properties

Lasue¹,

Levasseur-Regourd²,

Fray

et al. 2007

A&A

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“…Most of the Zodiacal light observed from near Earth originates from the dust in the approximate size range 1 to 100 µm located near ecliptic, at the distances from about 0.7 to 1.3 AU to the Sun [55,126]. Some observations point closer to the Sun and show that the visible Zodiacal light continues smoothly into the solar corona [139].…”

Section: Astronomical Observations Of Zodiacal Light and Cometsmentioning

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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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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“…For different objects, it differs only in the position of the maximum and minimum polarization and their values. Unlike the angular dependence, the spectral gradient of polarization, often called polarimetric color, differs for different objects: in the visible, polarization increases with wavelength for comets (Kolokolova et al 2004) but decreases for interplanetary dust (Levasseur-Regourd et al 2001), asteroids (Kiselev et al 1999;Ishiguro et al 1997), and the Moon (Dollfus & Bowell 1971). For debris disks, both tendencies were observed (Tamura et al 2006).…”

Section: Introductionmentioning

confidence: 99%

Effects of electromagnetic interaction in the polarization of light scattered by cometary and other types of cosmic dust

Kolokolova¹,

Kimura²

2010

A&A

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Context. We study how the electromagnetic interaction between the monomers in aggregates affects the polarization of cosmic dust. Aims. We aim to show that the electromagnetic interaction depends on the porosity and composition of the aggregates and contributes significantly to the spectral gradient of polarization (polarimetric color). The results may explain the observations of some comets that demonstrated atypical negative polarimetric color in the visible and also a reverse of the positive polarimetric color to the negative one in the near-infrared. Methods. We performed computer simulations of the light scattering by aggregates consisting of spheres made of a variety of materials: transparent, absorptive, and the material similar to that of the dust in comet Halley. We studied how the number of monomers covered by the electromagnetic wave at a single period (on the light path equal to one wavelength) affects their interaction by considering linear clusters of 2 and 10 monomers of radius of 0.1 μm. Results. Electromagnetic interaction between the monomers in aggregates depolarizes the light. The interaction becomes stronger if more monomers are covered by the electromagnetic wave at a single period. Thus, the porosity of aggregates influences their polarization. The electromagnetic interaction also depends on composition and is stronger for transparent materials. Conclusions. Electromagnetic interaction between the monomers in aggregates may explain why the polarimetric color of comet dust decreases as observations move from the visible to the near-infrared since a longer wavelength covers more monomers. It may also explain why some comets exhibit negative polarimetric color even in the visible; these comets may have more compact dust. Strong electromagnetic interaction resulted either from compactness or transparency of the material can explain the negative polarimetric color of interplanetary dust and debris disks and contribute to the polarization of asteroids. In general, the spectral dependence of polarization is a promising tool for studying the properties of cosmic dust particles, particularly their porosity.

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Optical and Thermal Properties of Interplanetary Dust

Cited by 41 publications

References 79 publications

Inferring the interplanetary dust properties

Inferring the interplanetary dust properties

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

Effects of electromagnetic interaction in the polarization of light scattered by cometary and other types of cosmic dust

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