Interstellar Dust Inside and Outside the Heliosphere
Harald Krueger, Eberhard Gruen

TL;DR
This paper reviews in-situ measurements of interstellar dust within the solar system, highlighting the properties, dynamics, and implications for understanding the local interstellar cloud through data from multiple spacecraft.
Contribution
It provides a comprehensive synthesis of spacecraft-based in-situ interstellar dust measurements and discusses their implications for LIC conditions and dust behavior.
Findings
Detection of large interstellar grains up to 10e-13 kg
Gas-to-dust ratio in LIC higher than astronomical estimates
Observed shift in dust flow direction in 2005
Abstract
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 10e-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…
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