Discovery of Jovian dust streams and interstellar grains by the Ulysses spacecraft

Grün, E.; Zook, H. A.; Baguhl, M.; Balogh, A.; Bame, S. J.; Fechtig, H.; Forsyth, R. J.; Manner, Mark; Horányi, M.; Kissel, J.; Lindblad, B. A.; Linkert, D.; Linkert, G.; Mann, Ingrid; McDonnell, J. A. M.; Morfill, G. E.; Phillips, J. L.; Polanskey, C.; Schwehm, G.; Siddique, N.; Staubach, P.; Švestka, Jiří; Taylor, Andrew D.

doi:10.1038/362428a0

Cited by 397 publications

(179 citation statements)

References 13 publications

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“…Gustafson & Misconi (1979) and Morfill & Grün (1979) calculated the trajectories of these charged ISD particles, and concluded that there are phases during the solar cycle where ISD will be focused towards the solar equatiorial plane and phases where the ISD will be defocused from the solar equatorial plane. In 1993, the first ISD particles were identified in the Ulysses dust data (Grün et al 1993). Later, data from Galileo, Helios, and the early mission phase of Cassini were also analyzed with respect to ISD (Altobelli et al , 2005(Altobelli et al , 2006).…”

Section: Introductionmentioning

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: Introductionmentioning

confidence: 99%

The flow of interstellar dust into the solar system

Sterken

Altobelli

Kempf

et al. 2012

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“…A stream of 'fresh ' interstellar dust entering the Solar System was detected by the Ulysses spacecraft (Grun et al 1993). Interstellar dust grains constitute most of the solid matter in the Galaxy.…”

Section: Introductionmentioning

confidence: 99%

UV-Vis spectroscopy of stardust

Fernandes¹,

Johnson²,

Bridges

et al. 2006

International Journal of Astrobiology

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: NASA's Stardust mission flew through the coma of comet Wild 2 in January 2004, capturing dust grains as it did so. The grains were returned safely to Earth in January 2006, and are in the process of being distributed to investigators. As members of the Spectroscopy Preliminary Examination Team, we are preparing to analyse Stardust grains. Our contribution is to measure the spectrum of the grains between 200 nm (in the near ultraviolet) and 800 nm (near infrared). The purpose of the measurement is to provide an additional technique for characterizing the grains, one that is complementary to other spectroscopic techniques and one that produces results that can be matched directly with spectra acquired remotely (with telescope or spacecraft instrumentation). As part of the preparation for analysis of Stardust materials, we are producing a database of spectra from appropriate minerals, and are honing the technique through analysis of primitive meteorites.

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“…For most of 1991 when Ulysses was inside 4 AU from the sun the impact rate of small particles was also low. However, within a few months of Jupiter fly-by, several bursts, in the impact rate were observed, which occurred with a remarkable periodicity of 28 it 3 days around Jupiter fly-by (Grün et al, 1993a). No periodic dust phenomena in interplanetary space have been known before for such small grains.…”

Section: Jupiter Dust Streamsmentioning

confidence: 99%

“…It arrives from the direction : ecliptic longitude 1 = 252° and latitude b = 2.5°. Grün et al (1993a) identified a significant flux of interstellar grains at the distance of Jupiter. In a more recent paper (Grün et al, 1993b) a detailed analysis of the extended Ulysses data set is given.…”

Section: · Interstellar Dustmentioning

confidence: 99%

Dust Measurements in the Outer Solar System

Grün¹

1994

Symp. - Int. Astron. Union

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Abstract. In-situ measurements of micrometeoroids provide information on the spatial distribution of interplanetary dust and its dynamical properties. Pioneers 10 and 11, Galileo and Ulysses spaceprobes took measurements of interplanetary dust from 0.7 to 18 AU distance from the sun. Distinctly different populations of dust particles exist in the inner and outer solar system. In the inner solar system, out to about 3 AU, zodiacal dust particles are recognized by their scattered light, their thermal emission and by in-situ detection from spaceprobes. These particles orbit the sun on low inclination (i < 30°) and moderate eccentricity (e < 0.6) orbits. Their spatial density falls off with approximately the inverse of the solar distance. Dust particles on high inclination or even retrograde trajectories dominate the dust population outside about 3 AU. The dust detector onboard the Ulysses spaceprobe identified interstellar dust sweeping through the outer solar system on hyperbolic trajectories. Within about 2 AU from Jupiter Ulysses discovered periodic streams of dust particles originating from within the jovian system.

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Discovery of Jovian dust streams and interstellar grains by the Ulysses spacecraft

Cited by 397 publications

References 13 publications

The flow of interstellar dust into the solar system

The flow of interstellar dust into the solar system

UV-Vis spectroscopy of stardust

Dust Measurements in the Outer Solar System

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