Cassini/Cosmic Dust Analyzer in situ dust measurements between Jupiter and Saturn

Altobelli, Nicolás; Dikarev, Valeri; Kempf, S.; Srama, R.; Helfert, S.; Moragas-Klostermeyer, G.; Roy, M.; Grün, E.

doi:10.1029/2006ja011978

Cited by 38 publications

(31 citation statements)

References 43 publications

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“…During its interplanetary cruise it measured interplanetary and interstellar grains (Baguhl et al 1995;Altobelli et al 2005). During the orbital tour of the Galileo mission (1996)(1997)(1998)(1999)(2000)(2001)(2002)(2003) Fig.…”

Section: The Galileo Missionmentioning

confidence: 99%

“…In this way ISD particles are repeatedly recycled through the galactic evolution process (Dorschner & Henning 1995). A&A 552, A130 (2013) Direct measurements of interstellar dust were made in situ in the solar system, using the dust instruments on spacecraft like Ulysses (Grün et al 1994;Baguhl et al 1996;Landgraf et al 2000;Krüger et al 2007), Galileo (Baguhl et al 1996;Altobelli et al 2005), Helios , and Cassini (Altobelli et al 2003). Ulysses provided the most extended data set of interstellar dust in the solar system from which an ISD size distribution was derived which is valid for the Ulysses observation period and orbit .…”

Section: Introductionmentioning

confidence: 99%

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The filtering of interstellar dust in the solar system

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Altobelli

Kempf

et al. 2013

A&A

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Context. Theoretical predictions demonstrate that small (<0.1 µm) interstellar grains are mostly excluded from reaching the planetary system by electromagnetic interactions in the heliopause region and in the inner heliosphere. Bigger interstellar grains have been recorded in the planetary system by dust measurements on board Ulysses and other spacecraft. It was found that the interstellar dust flux is modulated by the interplanetary magnetic field. Aims. The objective of this study is to analyze the heliospheric filtering of the interstellar dust flow through the solar system and throughout the solar cycle. In the heliosphere the dynamics of interstellar dust is governed by the gravitational pull of the Sun, by the repulsion of solar radiation, and by the deflection caused by the interaction of the charged interstellar dust (ISD) grains with the interplanetary magnetic field. These interactions are described by the parameters of the radiation pressure constant β and the charge-to-mass ratio Q/m, which depend on the particle's size, physical properties, and composition. A previous paper studied the flow characteristics of ISD moving through the solar system were studied. In this follow-up paper, we focus on how the ISD size distribution varies during its passage through the solar system. Methods. In a parametric study of 70 different β and Q/m values, we calculated interstellar dust trajectories starting at the boundary of the heliosphere with starting times spread over a complete solar cycle of 22 years. Results. As a result we obtained the interstellar dust flux and dust speed for these times and positions and demonstrate the effects of the filtering on the dust size distributions. The size distribution of ISD observed at any time and at any position in the planetary system is strongly modified from when it entered the heliosphere. Peaks in relative flux of 10 times the original flux possibly depend on the grain size and place and time in the solar system. We did a detailed study of three cases of the flux and size distribution of interstellar grains reaching the planets Saturn, Jupiter, and the main-belt asteroid Ceres. These cases are used to get a first idea of what a dust detector or collector on a mission to these bodies might see of ISD.

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Section: The Galileo Missionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

The filtering of interstellar dust in the solar system

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Altobelli

Kempf

et al. 2013

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“…Across different regions in the ISM, variations in extinction curves and emission/absorption features similarly suggest there may be large fluctuations in the relative abundance of large grains (Miville-Deschênes et al 2002;Gordon et al 2003;Dobashi et al 2008;Paradis et al 2009). The solar neighborhood, in particular, appears to exhibit an anomalous large-grain abundance (Krüger et al 2001;Frisch & Slavin 2003;Meisel et al 2002;Altobelli et al 2006Altobelli et al , 2007Poppe et al 2010). And Hopkins (2014b) suggested that this could explain some (but not all) of the variations in abundances observed within some star massive clusters.…”

Section: Introductionmentioning

confidence: 99%

The dynamics of charged dust in magnetized molecular clouds

Lee

Hopkins

Squire

2017

Monthly Notices of the Royal Astronomical Society

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We study the dynamics of large, charged dust grains in turbulent giant molecular clouds (GMCs). Massive dust grains behave as aerodynamic particles in primarily neutral dense gas, and thus are able to produce dramatic small-scale fluctuations in the dust-to-gas ratio. Hopkins & Lee (2016) directly simulated the dynamics of neutral dust grains in super-sonic MHD turbulence, typical of GMCs, and showed that the dust-to-gas fluctuations can exceed factor ∼ 1000 on small scales, with important implications for star formation, stellar abundances, and dust behavior and growth. However, even in primarily neutral gas in GMCs, dust grains are negatively charged and Lorentz forces are non-negligible. Therefore, we extend our previous study by including the effects of Lorentz forces on charged grains (in addition to drag). For small charged grains (sizes 0.1 µm), Lorentz forces suppress dust-to-gas ratio fluctuations, while for large grains (sizes 1 µm), Lorentz forces have essentially no effect, trends that are well explained with a simple theory of dust magnetization. In some special intermediate cases, Lorentz forces can enhance dust-gas segregation. Regardless, for the physically expected scaling of dust charge with grain size, we find the most important effects depend on grain size (via the drag equation) with Lorentz forces/charge as a second-order correction. We show that the dynamics we consider are determined by three dimensionless numbers in the limit of weak background magnetic fields: the turbulent Mach number, a dust drag parameter (proportional to grain size) and a dust Lorentz parameter (proportional to grain charge); these allow us to generalize our simulations to a wide range of conditions.

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“…(1) Altobelli et al (2006); (2) Grün et al (1994); (3) Baguhl et al (1996); (4) Landgraf et al (2000); (5) Krüger et al (2007); (6) Baguhl et al (1996), (7) Altobelli et al (2005); (8) Altobelli et al (2003); (9) Krüger et al (2004).…”

Section: Introductionmentioning

confidence: 99%

The flow of interstellar dust into the solar system

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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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Cassini/Cosmic Dust Analyzer in situ dust measurements between Jupiter and Saturn

Cited by 38 publications

References 43 publications

The filtering of interstellar dust in the solar system

The filtering of interstellar dust in the solar system

The dynamics of charged dust in magnetized molecular clouds

The flow of interstellar dust into the solar system

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