Mass-loading of the solar wind at 67P/Churyumov-Gerasimenko -- Observations and modelling

TL;DR

This study combines in-situ measurements and hybrid modeling to analyze how the solar wind interacts with comet 67P, revealing increased deflection with little deceleration during low activity, and identifying a localized energy transfer region.

Contribution

It provides the first detailed characterization of solar wind-comet interaction at 67P, highlighting the dominant deflection over deceleration and modeling the localized energy transfer region.

Findings

Solar wind deflection increases as the comet approaches the Sun.

Little to no deceleration of the solar wind is observed.

Energy transfer occurs in a localized region near the nucleus.

Abstract

Context. The first long-term in-situ observation of the plasma environment in the vicinity of a comet, as provided by the European Rosetta spacecraft. Aims. Here we offer characterisation of the solar wind flow near 67P/Churyumov-Gerasimenko (67P) and its long term evolution during low nucleus activity. We also aim to quantify and interpret the deflection and deceleration of the flow expected from ionization of neutral cometary particles within the undisturbed solar wind. Methods. We have analysed in situ ion and magnetic field data and combined this with hybrid modeling of the interaction between the solar wind and the comet atmosphere. Results. The solar wind deflection is increasing with decreasing heliocentric distances, and exhibits very little deceleration. This is seen both in observations and in modeled solar wind protons. According to our model, energy and momentum are transferred from the solar wind to the coma in a single region, centered on the nucleus, with a size in the order of 1000 km. This interaction affects, over larger scales, the downstream modeled solar wind flow. The energy gained by the cometary ions is a small fraction of the energy available in the solar wind. Conclusions. The deflection of the solar wind is the strongest and clearest signature of the mass-loading for a small, low-activity comet, whereas there is little deceleration of the solar wind.