Fig. 10


Two out of five microbalances, QCM1 and QCM5 show an increase in frequency during the bound orbit phase (Sept. 2014Feb. 2015) due to the dust mass accumulated on the quartz sensors. A strong anisotropy in the dust flux is inferred by comparing the much steeper frequency increase of QCM1, pointing toward the Sun (top panel) with respect to QCM5, pointing nadir (middle panel). The QCMs residual signal noise is due to the sensor thermal hysteresis. This effect is particularly evident for QCM1 for which the signal appears as a double line since GIADA commissioning after the Rosetta hibernation phase, giving a frequency error of 5 Hz, which is twice that of the other QCMs. The bottom panel shows the phase angle and the distance from the nucleus at which the data were acquired.

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