Effect of the mirror force on the collision rate due to energetic electron precipitation: Monte Carlo simulations

Abstract

We study the effect of the mirror force on the collision rate due to the energetic electron precipitation into the ionosphere. We solve the motion of individual precipitating electrons with the mirror force, where collisions with neutral gas are computed by the Monte Carlo method. By comparing the results with those without the mirror force, we examine the effect of the mirror force on the altitude profile of the ionization rate. First, we carry out simulations of mono-energetic precipitation of 3 keV electrons whose initial pitch angle is 70 degrees at 400 km at L = 6.45. We find that the collision rate peaks at around 120 km altitude and that the duration of the collision is scattered in time with a delay of about 5 ms compared with the result without mirror force. Next, we perform mono-energetic precipitation of the different energy and pitch angle ranges. Simulation results demonstrate that larger kinetic energy lowers the altitude profiles of the collision rate, consistent with previous studies. We also find that the upward motion of electrons bounced back from their mirror points results in the upward broadening of the altitude profile of the collision rate. Simulation results for electrons with kinetic energies above 100 keV show that a secondary peak of the collision rate is formed near the mirror point. The formation of the secondary peak can be explained by the stagnation of electrons around the mirror point at 130 km altitude, because the relatively long duration of staying in neutral gas increases the number of collisions. Simulation results show that under the precipitation of electrons in the kinetic energy range larger than tens of keV with the pitch angle close to the loss cone, the maximum collision rate in the altitude range lower than 100 km becomes one order of the magnitude smaller. The results of the present study suggest the importance of the mirror force for the precise modeling of ionospheric response due to the energetic electron precipitation caused by the pitch angle scattering through wave–particle interactions. Graphical Abstract

Improved Energy Resolution Measurements of Electron Precipitation Observed During an IPDP‐Type EMIC Event

“…Quantifying and characterizing energetic electron precipitation (EEP, i.e., >10 keV) is one of the requirements for a more complete description of solar forcing that can be used in coupled climate models (Duderstadt et al, 2021;Matthes et al, 2017;Nesse Tyssøy et al, 2021;Salice et al, 2024;Seppälä et al, 2015;van de Kamp et al, 2016). Electrons precipitating with energies >10 keV will typically deposit their energy in the atmosphere at altitudes of 100 km or below (Katoh et al, 2023;Turunen et al, 2009;Xu et al, 2020), leading to chemical and dynamical changes in the climate system (Andersson et al, 2012;Brasseur & Solomon, 2005;Guttu et al, 2021;Mironova et al, 2015;Orsolini et al, 2018;Sinnhuber et al, 2012). One mechanism that causes energetic electron precipitation is via scattering with EMIC waves (e.g., Denton et al, 2019;Millan & Thorne, 2007;Thorne & Kennel, 1971).…”