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Title:
Interstellar Dust in the Solar System
Authors:
Krüger, Harald; Landgraf, Markus; Altobelli, Nicolas; Grün, Eberhard
Affiliation:
AA(Max-Planck-Institut für Sonnensystemforschung; , Max-Planck-Institut für Kernphysik), AB(European Space Agency, ESOC), AC(NASA/JPL), AD(Max-Planck-Institut für Kernphysik; HIGP, University of Hawaii)
Publication:
Space Science Reviews, Volume 130, Issue 1-4, pp. 401-408 (SSRv Homepage)
Publication Date:
06/2007
Origin:
SPRINGER
Keywords:
Dust, Interstellar dust, Heliosphere, Interstellar matter
DOI:
10.1007/s11214-007-9181-7
Bibliographic Code:
2007SSRv..130..401K

Abstract

The Ulysses spacecraft has been orbiting the Sun on a highly inclined ellipse almost perpendicular to the ecliptic plane (inclination 79°, perihelion distance 1.3 AU, aphelion distance 5.4 AU) since it encountered Jupiter in 1992. The in situ dust detector on board continuously measured interstellar dust grains with masses up to 10‑13 kg, penetrating deep into the solar system. The flow direction is close to the mean apex of the Sun’s motion through the solar system and the grains act as tracers of the physical conditions in the local interstellar cloud (LIC). While Ulysses monitored 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. We review the results from in situ interstellar dust measurements in the solar system and present Ulysses’ latest interstellar dust data. These data indicate a 30° shift in the impact direction of interstellar grains w.r.t. the interstellar helium flow direction, the reason of which is presently unknown.
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