South–North and Radial Traverses through the Interplanetary Dust Cloud

Grün, E.; Staubach, P.; Baguhl, M.; Hamilton, D. P.; Zook, H. A.; Dermott, S. F.; Gustafson, B. Å. S.; Fechtig, H.; Kissel, J.; Linkert, D.; Linkert, G.; Srama, R.; Hanner, M. S.; Polanskey, C.; Horányi, M.; Lindblad, B. A.; Mann, Ingrid; McDonnell, J. A. M.; Morfill, G. E.; Schwehm, G.

doi:10.1006/icar.1997.5789

Cited by 116 publications

(105 citation statements)

References 28 publications

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“…Staubach (Staubach et al 1996;Grün et al 1997) upgraded Divine's model using new data from GALILEO and ULYSSES dust detectors. Solar radiation pressure was added as a second perturbation force and an additional population, Inter Stellar Dust (ISD), was implemented.…”

Section: Model Descriptionmentioning

confidence: 99%

Comparison of Meteoroid Flux Models for Near Earth Space

et al. 2007

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Over the last decade several new models for the sporadic interplanetary meteoroid flux have been developed. These include the Divine-Staubach and the Dikarev model. They typically cover mass ranges from 10 -18 g to 1 g and are applicable for model specific Sun distance ranges between 0.1 AU and 20 AU Near 1 AU averaged fluxes (over direction and velocities) for all these models are tuned to the well established interplanetary model by Grün et al. However, in many respects these models differ considerably. Examples are the velocity and directional distributions and the assumed meteoroid sources. In this paper flux predictions by the various models to Earth orbiting spacecraft are compared. Main differences are presented and analysed. The persisting differences even for near Earth space can be seen as surprising in view of the numerous ground based (optical and radar) and in situ (captured Inter Stellar Dust Particles, in situ detectors and analysis of retrieved hardware) measurements and simulations.

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Section: Model Descriptionmentioning

confidence: 99%

Comparison of Meteoroid Flux Models for Near Earth Space

et al. 2007

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“…About 30 years ago, analysis of the data obtained with the dust instruments flown on a couple of spacecraft suggested that ISD grains can cross the heliospheric boundary and penetrate deeply into the heliosphere (Bertaux and Blamont 1976;Wolf et al 1976). In the 1990s, this was undoubtedly demonstrated with the dust instrument carried by the Ulysses spacecraft: the Ulysses dust detector, which measured mass, speed and approach direction of the impacting grains, identified ISD grains with radius above 0.1 µm sweeping through the heliosphere (Grün et al 1993(Grün et al , 1994.…”

Section: Introductionmentioning

confidence: 99%

Interstellar Dust Inside and Outside the Heliosphere

Krüger

Grün

2008

Space Sci Rev

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In the early 1990s, after its Jupiter flyby, the Ulysses spacecraft identified interstellar dust in the solar system. Since then the in-situ dust detector on board Ulysses continuously monitored interstellar grains with masses up to 10 −13 kg, penetrating deep into the solar system. While Ulysses measured the interstellar dust stream at high ecliptic latitudes between 3 and 5 AU, interstellar impactors were also measured with the in-situ dust detectors on board Cassini, Galileo and Helios, covering a heliocentric distance range between 0.3 and 3 AU in the ecliptic plane. The interstellar dust stream in the inner solar system is altered by the solar radiation pressure force, gravitational focussing and interaction of charged grains with the time varying interplanetary magnetic field. The grains act as tracers of the physical conditions in the local interstellar cloud (LIC). Our in-situ measurements imply the existence of a population of 'big' interstellar grains (up to 10 −13 kg) and a gas-to-dust-mass ratio in the LIC which is a factor of 1.5-2 larger than the one derived from astronomical observations, indicating a concentration of interstellar dust in the very local interstellar medium. Until 2004, the interstellar dust flow direction measured by Ulysses was close to the mean apex of the Sun's motion through the LIC, while in 2005, the data showed a 30°shift, the reason of which is presently unknown. We review the results from spacecraft-based in-situ interstellar dust measurements in the solar system and their implications for the physical and chemical state of the LIC.

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“…The motion of the interstellar grains through the solar system was parallel to the flow of neutral interstellar hydrogen and helium gas, both traveling at a speed of 26 km s −1 (Baguhl et al 1995). The interstellar dust flow persisted at higher latitudes above the ecliptic plane, even over the poles of the Sun, whereas interplanetary dust is strongly depleted away from the ecliptic plane (Grün et al 1997).…”

Section: Large Interstellar Dust Grains In the Heliospherementioning

confidence: 98%

“…The Ulysses spacecraft detected impacts predominantly from a direction that was opposite to the expected impact direction of interplanetary dust grains. It was found that, on average, the impact velocities exceeded the local solar system escape velocity (Grün et al 1994). The motion of the interstellar grains through the solar system was parallel to the flow of neutral interstellar hydrogen and helium gas, both traveling at a speed of 26 km s −1 (Baguhl et al 1995).…”

Section: Large Interstellar Dust Grains In the Heliospherementioning

confidence: 99%

The Galactic Environment of the Sun: Interstellar Material Inside and Outside of the Heliosphere

et al. 2009

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Interstellar material (ISMa) is observed both inside and outside of the heliosphere. Relating these diverse sets of ISMa data provides a richer understanding of both the interstellar medium and the heliosphere. The galactic environment of the Sun is dominated by warm, low-density, partially ionized interstellar material consisting of atoms and dust grains. The properties of the heliosphere are dependent on the pressure, composition, radiation field, ionization, and magnetic field of ambient ISMa. The very low-density interior of the Local Bubble, combined with an expanding superbubble shell associated with star formation in the Scorpius-Centaurus Association, dominate the properties of the local interstellar medium (LISM). Once the heliosphere boundaries and interaction mechanisms are understood, interstellar gas, dust, pickup ions, and anomalous cosmic rays inside of the heliosphere can be directly compared to ISMa outside of the heliosphere. Our understanding of ISMa at the Sun is further enriched when the circumheliospheric interstellar material is compared to observations of other nearby ISMa and the overall context of our galactic environment. The IBEX mission will map the interaction region between the heliosphere and ISMa, and improve the accuracy of comparisons between ISMa inside and outside the heliosphere.

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South–North and Radial Traverses through the Interplanetary Dust Cloud

Cited by 116 publications

References 28 publications

Comparison of Meteoroid Flux Models for Near Earth Space

Comparison of Meteoroid Flux Models for Near Earth Space

Interstellar Dust Inside and Outside the Heliosphere

The Galactic Environment of the Sun: Interstellar Material Inside and Outside of the Heliosphere

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