Light scattering experiments with micron-sized dust aggregates: results on ensembles of SiO2 monospheres and of irregularly shaped graphite particles

Wurm, Gerhard; Relke, H.; Dorschner, J.; Krauß, Oliver

doi:10.1016/j.jqsrt.2004.05.036

Cited by 11 publications

(4 citation statements)

References 25 publications

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“…The temperature and polarization thus behave in opposite ways because a fluffy aggregate of small grains presents values of t close to the one of its equivalent volume sphere, whereas it scatters light in a similar way to one of its constituent grains as shown from numerical simulations (West 1991) and experimental simulations (Wurm et al 2004). …”

Section: Discussionmentioning

confidence: 89%

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: Discussionmentioning

confidence: 89%

Inferring the interplanetary dust properties

Lasue¹,

Levasseur-Regourd²,

Fray

et al. 2007

A&A

View full text Add to dashboard Cite

show abstract

“…In agreement with Xing & Hanner (1997), the temperature obtained for an aggregate of grains is lower than one of its constituent grains but is higher than the temperature of the equivalent volume sphere. The temperature and polarization thus behave in opposite ways because a fluffy aggregate of small grains present values of t close to the one of its equivalent volume sphere, whereas it scatters light in a way similar to one of its constituent grains as shown from numerical simulations (West 1991) and experimental simulations (Wurm et al 2004).…”

Section: Discussionmentioning

confidence: 96%

Inferring the interplanetary dust properties from remote observations and simulations

Lasue,

Levasseur-Regourd,

Fray

et al. 2016

Preprint

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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 light scattered and emitted, 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 particles 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 organics 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 solar distance, R, dependence of the temperature in R −0.45 different than the typical black body behavior. The heliocentric dependence of P α=90 • is interpreted as a progressive disappearance of solid organics (such as HCN polymers or amorphous carbon) towards the Sun. Conclusions.

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“…Furthermore, these are very common assumptions when studying the scattering properties of large clusters of particles [6,7].…”

Section: Derivation Of Spectral-domain Relationshipsmentioning

confidence: 99%

Spectral-Domain Integral Equation Method for Modeling the Scattering Properties of a Group of Planar Particles in the Presence of a Substrate

Lopushenko

2016

Comput Math Model

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Light scattering experiments with micron-sized dust aggregates: results on ensembles of SiO2 monospheres and of irregularly shaped graphite particles

Cited by 11 publications

References 25 publications

Inferring the interplanetary dust properties

Inferring the interplanetary dust properties

Inferring the interplanetary dust properties from remote observations and simulations

Spectral-Domain Integral Equation Method for Modeling the Scattering Properties of a Group of Planar Particles in the Presence of a Substrate

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