Kim K., D. Lee, (2014), Magnetopause structure favorable for radiation belt electron loss, J. Geophys. Res. [Space Physics], 119, 5495-5508, doi:10.1002/2014JA019880

## Abstract

Abstract Magnetopause shadowing is regarded as one of the major reasons for the loss of relativistic radiation belt electrons, although this has not yet been fully validated by observations. Previous simulations on this process assumed that all of the electrons encountering the magnetopause are simply lost into the magnetosheath just as ring current ions can be and did not examine details of the particle dynamics across and inside the magnetopause which has a finite thickness. In this paper, we perform test particle orbit calculations based on a simplified one-dimensional magnetopause model to demonstrate specifically how relativistic electrons arriving at the prenoon side of the magnetopause can be lost. The calculation results indicate that the loss process is determined by two factors: (i) a gradient of the magnetic field magnitude, B, along the magnetopause and (ii) a component of the magnetic field normal to the magnetopause. First, without a normal component of the magnetic field as in a tangential discontinuity, electrons can cross the magnetopause by the magnetic gradient drift motion due to the existence of B-gradient along the magnetopause. The minimum kinetic energies for loss decrease with increasing B-gradient along the magnetopause induced by the enhanced solar wind dynamic pressure. However, this process is not too strong in the sense that electrons have to drift rather a long distance along the magnetopause before entering the magnetosheath unless the B-gradient along the magnetopause is unusually strong, or the particle energy is very high like above 3 MeV. In contrast, if a normal component of the magnetic field exists inside the magnetopause, as in a rotational discontinuity, electrons can cross the magnetopause far more easily along the guided field line inside the magnetopause. This is effective for even a very small magnitude of normal component field such as somewhat less than 1 nT regardless of its direction and for a rather low energy of particles such as 0.5 MeV. Also, the loss occurs over more than half of the pitch angle domain, i.e., in the range between ~80° and 180° or 0° and ~100°, depending on the direction of normal component. Therefore, we suggest that radiation belt electron loss by the magnetopause shadowing process can be substantial (or can be effective) when a substantial area of the magnetopause is given a finite normal magnetic field component as well as B-gradient along the magnetopause.## Authors (sorted by name)

Kim Lee## Journal / Conference

Journal Of Geophysical Research (Space Physics)## Acknowledgments

The data used for this paper were obtained from numerical calculations and are available from the corresponding author upon request. This research was supported by the Study of Near‐Earth Effects by the CME/HSS project and basic research funding from KASI. The work at Chungbuk National University was supported by a NSL grant (NRF‐2011‐0030742) from the National Research Foundation of Korea.## Bibtex

@article{doi:10.1002/2014JA019880,
author = {Kim, Kyung-Chan and Lee, Dae-Young},
title = {Magnetopause structure favorable for radiation belt electron loss},
journal = {Journal of Geophysical Research: Space Physics},
volume = {119},
number = {7},
pages = {5495-5508},
year = {2014},
keywords = {magnetopause shadowing, relativistic electron loss, test particle orbit calculation},
doi = {10.1002/2014JA019880},
url = {https://agupubs.onlinelibrary.wiley.com/doi/abs/10.1002/2014JA019880},
eprint = {https://agupubs.onlinelibrary.wiley.com/doi/pdf/10.1002/2014JA019880},
abstract = {Abstract Magnetopause shadowing is regarded as one of the major reasons for the loss of relativistic radiation belt electrons, although this has not yet been fully validated by observations. Previous simulations on this process assumed that all of the electrons encountering the magnetopause are simply lost into the magnetosheath just as ring current ions can be and did not examine details of the particle dynamics across and inside the magnetopause which has a finite thickness. In this paper, we perform test particle orbit calculations based on a simplified one-dimensional magnetopause model to demonstrate specifically how relativistic electrons arriving at the prenoon side of the magnetopause can be lost. The calculation results indicate that the loss process is determined by two factors: (i) a gradient of the magnetic field magnitude, B, along the magnetopause and (ii) a component of the magnetic field normal to the magnetopause. First, without a normal component of the magnetic field as in a tangential discontinuity, electrons can cross the magnetopause by the magnetic gradient drift motion due to the existence of B-gradient along the magnetopause. The minimum kinetic energies for loss decrease with increasing B-gradient along the magnetopause induced by the enhanced solar wind dynamic pressure. However, this process is not too strong in the sense that electrons have to drift rather a long distance along the magnetopause before entering the magnetosheath unless the B-gradient along the magnetopause is unusually strong, or the particle energy is very high like above 3 MeV. In contrast, if a normal component of the magnetic field exists inside the magnetopause, as in a rotational discontinuity, electrons can cross the magnetopause far more easily along the guided field line inside the magnetopause. This is effective for even a very small magnitude of normal component field such as somewhat less than 1 nT regardless of its direction and for a rather low energy of particles such as 0.5 MeV. Also, the loss occurs over more than half of the pitch angle domain, i.e., in the range between ~80° and 180° or 0° and ~100°, depending on the direction of normal component. Therefore, we suggest that radiation belt electron loss by the magnetopause shadowing process can be substantial (or can be effective) when a substantial area of the magnetopause is given a finite normal magnetic field component as well as B-gradient along the magnetopause.}
}