Interactions with Electromagnetic Radiation: Theory and Laboratory Simulations

Gustafson, B. Å. S.; Kolokolova, L.; Xu, Yu-lin; Greenberg, J. Mayo; Stognienko, R.

doi:10.1007/978-3-642-56428-4_11

Cited by 16 publications

(11 citation statements)

References 135 publications

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“…The scattering efficiency can be calculated for spherical particles by Mie-scattering theory and for particles that are much smaller than the wavelength, Rayleigh scattering can be applied (Burns et al 1979). For nonspherical particles, elaborate scattering algorithms have often been applied, and even laboratory simulations are used to obtain relevant Q pr values for determining relevant β values (see Gustafson et al 2001, for a review). Kimura & Mann (1999) calculated β-curves for fluffy carbon and silicate particles (Fig.…”

Section: Particle Properties β and Q/mmentioning

confidence: 99%

The flow of interstellar dust into the solar system

Sterken

Altobelli

Kempf

et al. 2012

A&A

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Context. Interstellar dust (ISD) is a major component in the formation and evolution of stars, stellar systems, and planets. Astronomical observations of interstellar extinction and polarization, and of the infrared emission of the dust, are the most commonly used technique for characterizing interstellar dust. Besides this, the interstellar dust from the local interstellar cloud enters the solar system owing to the relative motion of the Sun with respect to this cloud. Once in the solar system, in-situ observations can be made by spacecraft using impact ionization detectors and time-of-flight spectrometers like the ones flown on the Cassini, Ulysses, and Galileo, spacecrafts. Also a sample return can be done, as in the Stardust mission. Once in the solar system, the trajectories of these dust grains are shaped by gravitational, solar radiation pressure, and Lorentz forces. The Lorentz forces result from the interaction of the charged dust particles with the interplanetary magnetic field. The ISD densities in the solar system thus depend both on the location in the solar system and on time, correlated to the solar cycle. Aims. This paper aims at giving the reader insight into the flow patterns of ISD when it moves through the solar system. This is useful for designing future in-situ or sample return missions or for knowing whether for specific missions, simplified assumptions can be used for the dust flux and direction, or whether full simulations are needed. Methods. We characterize the flow of ISD through the solar system using simulations of the dust trajectories. We start from the simple case without Lorentz forces and expand to the full simulation. We pay attention to the different ways of modeling the interplanetary magnetic field and discuss the influence of the dust parameters on the resulting flow patterns. Dust densities, fluxes, and directionalities are derived from the trajectory simulations. Different graphics representations are used to gain insight into the flow patterns. As an illustration of how the model can be used, we predict the fluxes and directionalities of the ISD for the Cassini mission. Results. The characteristics of the flow of ISD through the solar system have been investigated to gain insight in the patterns of the flow. The modeling can also be used for predicting dust fluxes for different space missions or planets, and for understanding spacecraft measurements, such as those from Ulysses, Cassini, and Stardust.

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Section: Particle Properties β and Q/mmentioning

confidence: 99%

The flow of interstellar dust into the solar system

Sterken

Altobelli

Kempf

et al. 2012

A&A

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“…The radiation pressure on fluffy dust grains has been estimated by numerical computations based on microwave analogue measurements or based on Mie theory with a combination of effective medium approximations (EMAs), such as the MaxwellGarnett mixing rule and the Bruggeman mixing rule (Mukai et al 1992, Gustafson 1994, Wilck and Mann 1996, Kimura and Mann 1999a, Gustafson et al 2001. The application of EMAs relies on the assumption that a fluffy grain can be treated as a sphere having an average refractive index of constituent material and vacuum.…”

Section: Introductionmentioning

confidence: 99%

Radiation Pressure and the Poynting–Robertson Effect for Fluffy Dust Particles

Kimura

Okamoto

Mukai

2002

Icarus

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“…those that use Discrete Dipole Approximation, DDA (Lumme & Rahola, 1994;Wolff et al, 1998;Voshchinnikov et al, 2007;Shen et al, 2008), and experiments (Kolokolova & Gustafson, 2001) show that even for xRe(m) ~1 effective medium theories provide reasonable results. The best accuracy can be obtained for cross sections and the worst for polarization, especially at phase angles smaller than 50° and larger than 120°.…”

Section: Electrostatic Approximation: Effective Medium Theoriesmentioning

confidence: 99%

“…Due to this, the field of light scattering by cosmic dust has always been at the frontier of the study of interaction of electromagnetic waves with non-spherical and inhomogeneous particles. It has inspired publication of the scholarly books by van de Hulst (1957), Schuerman (1980, Kokhanovsky (2001), Hovenier et al (2004), Voshchinnikov (2004, Borghese et al (2010), and Mishchenko et al (2000Mishchenko et al ( , 2002Mishchenko et al ( , 2010 and numerous book chapters, e.g., Mukai (1989), Lien (1991), Gustafson (1999), Gustafson et al (2001), Kolokolova et al (2004a, b). To consider the scattering of electromagnetic waves by an object of complex structure, we will determine this object as a configuration of discrete finite constituents.…”

Section: Introductionmentioning

confidence: 99%