The Solar Wind Interaction with (1) Ceres: The Role of Interior Conductivity

Abstract

As a potential “ocean world,” (1) Ceres’ interior may possess relatively high electrical conductivities on the order of 10−4–100 S m−1, suggesting that the solar wind interaction with Ceres may differ from other highly resistive objects such as the Moon. Here, we use a hybrid plasma model to quantify the solar wind interaction with Ceres over a range of scenarios for Ceres’ internal conductivity structure and the upstream solar wind and interplanetary magnetic field (IMF) conditions. Internal models for Ceres include one-, two-, and three-layer conductivity structures that variously include a crust, mantle, and/or subsurface ocean, while modeled solar wind conditions include a nominal case, a high IMF case, and an “extreme” space weather case. To first order, Ceres’ interaction with the solar wind is governed by the draping and enhancement of the IMF over its interior, whether from a moderate-conductivity mantle or a high-conductivity ocean. In turn, IMF draping induces compressional wings in the solar wind density and deceleration in the solar wind speed outside of Ceres. Together, all three effects are readily observable by a hypothetical orbital or landed mission with standard plasma and magnetic field instrumentation. Finally, we also consider the possible effects of unipolar induction within Ceres, which has been previously suggested as a mechanism for conducting bodies in the solar wind. Our model results show that the efficacy of unipolar induction is highly suppressed by the slow magnetic field-line diffusion through Ceres’ interior and, thus, is not a significant contributor to Ceres’ overall interaction with the solar wind.

Unveiling the 3D Structure of Magnetosheath Jets

“…Amitis has been extensively applied to study plasma interactions with various planetary bodies including the Moon, Mercury, Ganymede, Mars, Comets, and several asteroids (e.g., Fatemi et al, 2017;Fuqua-Haviland et al, 2019;Fatemi et al, 2020;Aizawa et al, 2021;Poppe et al, 2021;Rasca et al, 2022;Fatemi et al, 2022;Shi et al, 2022;X.-D. Wang et al, 2023;Poppe & Fatemi, 2023;Gunell et al, 2024). In addition, its results have been successfully validated through comparison with spacecraft observations (e.g., Fatemi et al, 2017Fatemi et al, , 2020Aizawa et al, 2021;Rasca et al, 2022;Fatemi et al, 2022;X.-D. Wang et al, 2023), theories (Fuqua-Haviland et al, 2019), and other kinetic and magnetohydrodynamic (MHD) models (Fatemi et al, 2017;Aizawa et al, 2021).…”

Unveiling the 3D Structure of Magnetosheath Jets

“…Amitis has been extensively applied to study plasma interactions with various planetary bodies including the Moon, Mercury, Ganymede, Mars, and several asteroids (e.g., Fatemi et al, 2017;Fuqua-Haviland et al, 2019;Fatemi et al, 2020;Aizawa et al, 2021;Poppe et al, 2021;Rasca et al, 2022;Fatemi et al, 2022;Shi et al, 2022;X.-D. Wang et al, 2023;Poppe & Fatemi, 2023). In addition, its results have been successfully validated through comparison with spacecraft observations (e.g., Fatemi et al, 2017Fatemi et al, , 2020Aizawa et al, 2021;Rasca et al, 2022;Fatemi et al, 2022;X.-D. Wang et al, 2023), theories (Fuqua-Haviland et al, 2019), and other kinetic and Magnetohydrodynamic (MHD) models (Fatemi et al, 2017;Aizawa et al, 2021).…”