Geoscience Letters

Official Journal of the Asia Oceania Geosciences Society (AOGS)

Geoscience Letters Cover Image
Open Access

Introduction to the thematic series “Coupling of the magnetosphere–ionosphere system”

Geoscience LettersOfficial Journal of the Asia Oceania Geosciences Society (AOGS)20174:27

https://doi.org/10.1186/s40562-017-0092-5

Received: 10 November 2017

Accepted: 14 November 2017

Published: 20 November 2017

Abstract

This thematic series contains 4 papers mostly presented at the 2016 AOGS meeting in Beijing. The four papers investigate four key regions in the magnetosphere–ionosphere coupling process: mid-tail magnetosphere, near-Earth magnetosphere, inner magnetosphere, and the polar ground region. Guo et al. (Geosci Lett 4:18, 2017) study the current system in reconnection region using 2.5D particle-in-cell simulations. Yao et al. (Geosci Lett 4:8, 2017) use conjugate measurements from ground auroral imagers and in situ THEMIS spacecraft to reveal the mechanism for the wave-like auroral structures prior to substorm onset. Zhang et al. (Geosci Lett 4:20, 2017) investigate the profiles of resonance zone and resonant frequency in the Landau resonance between radiation belt electrons and magnetosonic waves and between protons and cyclotron waves. Rae et al. (Geosci Lett 4:23, 2017) determine the relative timing between sudden increases in amplitude, or onsets, of different ultra-low-frequency wave bands during substorms.

Introduction

The dynamic coupling between the magnetosphere and the ionosphere system is crucial for understanding energy dissipation in the Earth system and in both solar system planets and exoplanets. The Earth’s polar ionosphere couples to the entire magnetosphere; the distant tail > 25 R E, near/mid-Earth magnetotail 6.6–25 R E, and inner magnetosphere < 6.6 R E. Particle acceleration, field-aligned current generation, and ground magnetic perturbations are the most pivotal and challenging in understanding how the magnetosphere–ionosphere system is coupled. The past two decades have seen the development and launch of a number of space missions and deployment of ground stations dedicated to the investigation of a particular link in the chain of interactions between magnetosphere and ionosphere. With these new assets, it is now possible to understand the energy conversion process between magnetosphere and ionosphere on both global and localized scales with conjugate measurements in all key regions, i.e., the mid-magnetotail, near-Earth magnetotail, ionosphere, and Earth’s polar ground.

The thematic series of Geoscience Letters are mostly based on presentations from the session on the same topic (ST06: Magnetosphere–Ionosphere Coupling Dynamics) organized at the Asia Oceania Geosciences Society (AOGS) General Assembly held in Beijing during July 31–August 5, 2016. The papers are organized in the order from the outer magnetosphere to the inner magnetosphere and the ionosphere.

Mid-tail magnetosphere

Energy in driving terrestrial magnetospheric dynamics originates from the solar wind and is stored in the magnetosphere via magnetopause reconnection (Dungey 1961). In the magnetotail, reconnection is essential in energizing particles, producing high-speed flows, and the formation of plasmoids. How electrons are accelerated via reconnection and how reconnection outflow drives magnetotail dynamics are two fundamental topics in terrestrial magnetosphere field.

From 2.5D particle-in-cell (PIC) simulations, Guo et al. (2017) examine current systems forming near the electron separatrix and investigating a non-gyrotropic electron distribution. These authors suggest that a dramatic change in the orientation of the electron velocity could be a diagnostic to detect the electron separatrix. In the reconnection exhaust region, Guo et al. (2017) show that ions are the main carriers for the out-of-plane current, while the parallel current is mainly carried by electrons.

Near-Earth and inner magnetosphere

Reconnection outflow from night-side tail reconnection propagates from mid-tail to near-Earth magnetotail and inner magnetosphere. The propagation of these flows causes perturbations of plasma and fields, which can lead to particle energization in the inner region.

A major impact of the reconnection outflow is caused by its braking and deceleration in the near-Earth magnetotail. These include flux pileup (e.g., Shiokawa et al. 1997) and the development of plasma instabilities (e.g., Lui 1991) in the inner magnetosphere. By analyzing simultaneous measurements from the near-Earth THEMIS probes (Angelopoulos 2008) and ground auroral imagers, Yao et al. (2017) reveal that a kinetic-scale ballooning instability was excited at the arrival of a reconnection outflow. This caused the development of wave-like auroral structures in the atmosphere. Their analysis shows consistent wavelength from aurora and in situ measurements. Moreover, they also present similar wave-like auroral feature at Saturn and Jupiter, which may imply that a common process exists at other planets.

Zhang et al. (2017) investigate the profiles of resonance zone and resonant frequency in the Landau resonance between radiation belt electrons and magnetosonic waves and between protons and cyclotron waves. Their results demonstrate that resonant interactions between magnetosonic waves and magnetospheric charged particles depend heavily on L-shell, wave normal angle, kinetic energy, and equatorial pitch angle of the particles. Resonance zones for the Landau resonance between magnetosonic waves and radiation belt electrons are confined to a very narrow (mostly less than 1°) extent of magnetic latitude, which tends to shift to lower latitudes with increasing equatorial pitch angle and decreasing electron energy.

Ground magnetic perturbation

Measurements of ground magnetic perturbations provide a unique view for understanding the global development of ionospheric and magnetospheric current system during a substorm. Rae et al. (2017) determine the relative timing between sudden increases in amplitude, or onsets, of different ultra-low-frequency (ULF) wave bands during substorms. They show that differing onset times and spatial expansion exist for Pi1, Pi1-2, and Pi2 waves in the ionosphere during substorms. Their results demonstrate how careful analysis of ULF waves during substorm onset can provide vital information on the physical processes occurring and time history of these processes through substorm onset.

Declarations

Authors’ contributions

All the authors acted as Guest Editors for the contributed papers. The Introduction was first drafted by ZY but all the authors read and agreed the contents. All authors read and approved the final manuscript.

Acknowledgements

We thank all the authors who presented the papers at the AOGS meeting and contributed to this thematic collection. We also thank reviewers for improving the quality of papers. ZHY is a Marie-Curie COFUND research fellow, cofunded by EU.

Competing interests

The authors declare that they have no competing interests.

Availability of data and materials

All the papers introduced here have been published.

Funding

Asia and Oceania Geoscience Society contributed Article Processing Charges for this Introduction, as well as most of the papers.

Publisher’s Note

Springer Nature remains neutral with regard to jurisdictional claims in published maps and institutional affiliations.

Open AccessThis article is distributed under the terms of the Creative Commons Attribution 4.0 International License (http://creativecommons.org/licenses/by/4.0/), which permits unrestricted use, distribution, and reproduction in any medium, provided you give appropriate credit to the original author(s) and the source, provide a link to the Creative Commons license, and indicate if changes were made.

Authors’ Affiliations

(1)
Laboratoire de Physique Atmospherique et Planetaire, STAR Institute, Universite de Liege
(2)
Goddard Space Flight Center, NASA
(3)
UCL Mullard Space Science Laboratory
(4)
INPE

References

  1. Angelopoulos V (2008) The THEMIS mission. Space Sci Rev 141(1):5–34View ArticleGoogle Scholar
  2. Dungey JW (1961) Interplanetary magnetic field and the auroral zones. Phys Rev Lett 6:47–48. https://doi.org/10.1103/PhysRevLett.6.47 View ArticleGoogle Scholar
  3. Guo RL, Pu ZY, Wei Y (2017) Current structure and flow pattern on the electron separatrix in reconnection region. Geosci Lett 4:18. https://doi.org/10.1186/s40562-017-0085-4 View ArticleGoogle Scholar
  4. Lui ATY (1991) A synthesis of magnetospheric substorm models. J Geophys Res Space Phys 96(A2):1849–1856View ArticleGoogle Scholar
  5. Rae IJ, Murphy KR, Watt CEJ, Mann IR, Yao ZH, Kalmoni NME, Forsyth C, Milling DK (2017) Using ultra-low frequency waves and their characteristics to diagnose key physics of substorm onset. Geosci Lett 4:23. https://doi.org/10.1186/s40562-017-0089-0 View ArticleGoogle Scholar
  6. Shiokawa K, Baumjohann W, Haerendel G (1997) Braking of high-speed flows in the near-Earth tail. Geophys Res Lett 24(10):1179–1182View ArticleGoogle Scholar
  7. Yao ZH, Pu ZY, Rae IJ, Radioti A, Kubyshkina MV (2017) Auroral streamer and its role in driving wave-like pre-onset aurora. Geosci Lett 4:8. https://doi.org/10.1186/s40562-017-0075-6 View ArticleGoogle Scholar
  8. Zhang WX, Zhou RX, Yi J, Gu XD, Ni BB, Zheng CY, Hua M (2017) Resonance zones for interactions of magnetosonic waves with radiation belt electrons and protons. Geosci Lett 4:20. https://doi.org/10.1186/s40562-017-0086-3 View ArticleGoogle Scholar

Copyright

© The Author(s) 2017