Eberhard Grün

TL;DR: In this article, the gas-to-dust mass ratio for the cloud surrounding the solar system was derived by combining spectroscopic observations of the gas phase abundances in the nearest interstellar clouds.

TL;DR: In this article, the mass and size distribution of the particles from the rms voltage of the induced noise and the impulse rate were determined based on the assumption that the voltage induced on the antenna is proportional to the mass of the colliding particle, and the results showed that the mass distribution varies as m −3, and most of the detected particles had radii in the range from 0.3 to 3 μm.

TL;DR: In this paper, the cloud potential V and dust potential U in dusty clouds are calculated for two limiting theoretical cases between which actual cases are expected to exist, and the results show that the values of V and U are strongly dependent on the character of the internal plasma and that, most of the time during which internal plasma retains its non-Maxwellian character, the creation of double layers and the occurrence of transitions with considerable readjustments of the cloud structure are possible.

TL;DR: In this article, the authors used an approximated theoretical instead of the measured impact velocity to derive the mass of interstellar grains from the Ulysses and Galileo in situ data, and the revised mass distributions are steeper and contain less large grains than the ones that use measured impact velocities, but large grains still contribute significantly to the overall mass of the detected grains.

TL;DR: The Rosetta probe, orbiting Jupiter-family comet 67P/Churyumov-Gerasimenko, has been detecting individual dust particles of mass larger than 10−10 kg by means of the GIADA dust collector and the OSIRIS Wide Angle Camera and Narrow Angle Camera as mentioned in this paper.