Physics of Zodiacal Dust

Gustafson, B. Å. S.

doi:10.1146/annurev.ea.22.050194.003005

Cited by 218 publications

(217 citation statements)

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“…(3)). The ratio of the Lorentz force to the effective gravitation is given as function of particle size a and distance to the Sun r. Assumed is a β-particle-size dependency (β-curve) for astronomical silicates, from Gustafson (1994). The ratio of gravity and radiation pressure force is 1 for particles of sizes of approximately 0.1 μm and 0.35 μm, which can be seen in Fig.…”

Section: Lorentz Forcesmentioning

confidence: 99%

“…The β-curve for astronomical silicates (Gustafson 1994) is adapted to the Ulysses observations to have a maximum β-value of β max = 1.6 (Landgraf et al 1999a). This curve (see Fig.…”

Section: Particle Properties β and Q/mmentioning

confidence: 99%

“…Kimura & Mann (1999) showing the influence of porosity on the β-value of the dust, namely a flattening of the curve. Kimura & Mann (1999) and one "adapted" astronomical silicates curve (Gustafson 1994). The β-curves relate the β-parameter of a material to its size.…”

Section: Particle Properties β and Q/mmentioning

confidence: 99%

“…A bulk particle size of 0.3 μm was found, assuming that they are "astronomical silicates" as described in Gustafson (1994). Linde & Gombosi (2000) postulates that ISD smaller than about 0.2 μm would be filtered at the heliopause, so there is a filtering of particles at entry into the solar system.…”

Section: Introductionmentioning

confidence: 99%

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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: Lorentz Forcesmentioning

confidence: 99%

“…The β-curve for astronomical silicates (Gustafson 1994) is adapted to the Ulysses observations to have a maximum β-value of β max = 1.6 (Landgraf et al 1999a). This curve (see Fig.…”

Section: Particle Properties β and Q/mmentioning

confidence: 99%

Section: Particle Properties β and Q/mmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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The flow of interstellar dust into the solar system

Sterken

Altobelli

Kempf

et al. 2012

A&A

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“…Using momentum-transfer cross-sections of particles of mass m from the stellar radiation, C pr , and from the stellar wind, C sw , the ratios β and β sw are given by (Gustafson 1994;Minato et al 2004;2006),…”

Section: Equation Of Motionmentioning

confidence: 99%

Dust ring formation due to sublimation of dust grains drifting radially inward by the Poynting–Robertson drag: An analytical model

Kobayashi

Watanabe

Kimura

et al. 2009

Icarus

107

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Dust particles exposed to the stellar radiation and wind drift radially inward by the Poynting-Robertson (P-R) drag and pile up at the zone where they begin to sublime substantially. The reason they pile up or form a ring is that their inward drifts due to the P-R drag are suppressed by stellar radiation pressure when the ratio of radiation pressure to stellar gravity on them increases during their sublimation phases. We present analytic solutions to the orbital and mass evolution of such subliming dust particles, and find their drift velocities at the pileup zone are almost independent of their initial semimajor axes and masses. We derive analytically an enhancement factor of the number density of the particles from their drift velocities at the outer edge of the sublimation zone.We show that the formula of the enhancement factor reproduces well numerical simulations in the previous studies. The enhancement factor for spherical dust particles of silicate and carbon extends from 3 to more than 20 at stellar luminosities L = 0.8-500L , where L is solar luminosity. Although the enhancement factor for fluffy dust particles is smaller than that for spherical particles, sublimating particles inevitably form a dust ring as long as their masses decrease faster than their surface areas during sublimation. The formulation is applicable to dust ring formation for arbitrary shape and material of dust in dust-debris disks as well as in the Solar System.-4 -

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Pinpointing Planets in Circumstellar Disks

Quillen

2010

Formation and Evolution of Exoplanets

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A crowning achievement in mathematical science was the prediction by Urbain Le Verrier and John Couch Adams in 1845 of a previously unknown planet that was then subsequently discovered. Irregularities in Uranus's orbit were elegantly explained as being due to a single massive object exerting perturbations on Uranus and the position of the object in the sky was predicted. The planet Neptune was subsequently detected by Johann Gottfried Galle at the Berlin Observatory (cf.[1]). Planets can not only perturb each other, as outlined in the original perturbative theory by Laplace, but also perturb the orbits of smaller particles such as dust that can be much more numerous and so can reemit a detectable fraction of the host star luminosity. Disk morphology can provide dynamical evidence for massive bodies that can be subsequently discovered from direct observations. We can refer to historical examples in our solar system. For example, the prediction of a satellite in the Encke gap in Saturn's rings based on wavy edges seen in the gap [2], was followed by the discovery of the satellite, Pan [3].In this chapter, a broad base of dynamical work relating circumstellar disk morphology to underlying planetary architecture is reviewed. The existence of a planet was predicted on the basis of its interactions with the circumstellar disk in the Fomalhaut system [4] at a semimajor axis of 119 AU. Subsequently, a planet was discovered with an estimated semimajor axis of 115 AU [5], only 4 AU lower than predicted. This is the first planet whose existence was successfully predicted from its interactions with the surrounding circumstellar disk (see Figure 2.1). discovery illustrates that we can, in some cases, predict the presence of planetary bodies from their interactions with disk material. The discrepancies between the predicted planetary orbit and mass from those inferred from observations are and will continue to be interesting. In probing them, we will improve our theoretical understanding and extend our capabilities so that we can accurately infer planetary system architecture at levels below the concurrent detection limits. In this chapter, we discuss some of the broad foundation of work that this prediction and others are built Formation and Evolution of Exoplanets. Edited by Rory Barnes

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Physics of Zodiacal Dust

Cited by 218 publications

References 0 publications

The flow of interstellar dust into the solar system

The flow of interstellar dust into the solar system

Dust ring formation due to sublimation of dust grains drifting radially inward by the Poynting–Robertson drag: An analytical model

Pinpointing Planets in Circumstellar Disks

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