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Magnetohydrodynamic Oscillations in the Solar Corona and Earth’s Magnetosphere: Towards Consolidated Understanding

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Abstract

Magnetohydrodynamic (MHD) oscillatory processes in different plasma systems, such as the corona of the Sun and the Earth’s magnetosphere, show interesting similarities and differences, which so far received little attention and remain under-exploited. The successful commissioning within the past ten years of THEMIS, Hinode, STEREO and SDO spacecraft, in combination with matured analysis of data from earlier spacecraft (Wind, SOHO, ACE, Cluster, TRACE and RHESSI) makes it very timely to survey the breadth of observations giving evidence for MHD oscillatory processes in solar and space plasmas, and state-of-the-art theoretical modelling. The paper reviews several important topics, such as Alfvénic resonances and mode conversion; MHD waveguides, such as the magnetotail, coronal loops, coronal streamers; mechanisms for periodicities produced in energy releases during substorms and solar flares, possibility of Alfvénic resonators along open field lines; possible drivers of MHD waves; diagnostics of plasmas with MHD waves; interaction of MHD waves with partly-ionised boundaries (ionosphere and chromosphere). The review is mainly oriented to specialists in magnetospheric physics and solar physics, but not familiar with specifics of the adjacent research fields.

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Notes

  1. For example, the nominal cadence time of the Atmospheric Imaging Assembly on the Solar Dynamics Observatory is 12 seconds, while there is a technical possibility to reduce it to 2 seconds for selected wavelength channels (Lemen et al. 2012). The High Resolution Coronal Imager (Hi-C) on a sounding rocket had the cadence of 5.57 s (Kobayashi et al. 2014).

  2. The rapidly-propagating waves of emission intensity, detected with the Solar Eclipse Coronal Imaging System (SECIS) by Williams et al. (2002) and Katsiyannis et al. (2003) could also be produced by kink waves by the variation of the apparent column depth (Cooper et al. 2003a,b).

  3. http://ccmc.gsfc.nasa.gov/modelweb/.

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Acknowledgements

This review is based upon the activities of the international science team “MHD oscillations in the solar corona and Earth’s magnetosphere: towards consolidated understanding” supported by the International Space Science Institute, Bern, Switzerland. The authors would like to thank Dr N. Nishitani and Dr A. Yoshikawa for the valuable discussions. The authors acknowledge the support by the STFC Warwick Astrophysics Consolidated Grant ST/L000733/1 (VMN, GN); the European Research Council under the SeismoSun Research Project No. 321141 (VMN), BK21 plus program through the National Research Foundation funded by the Ministry of Education of Korea (DHL, VMN); the Leverhulme Trust (GV); the János Bolyai Research Scholarship of the Hungarian Academy of Sciences (BH); grant P209/12/0103 and 16-13277S (GA CR) (MK, PJ); an Odysseus grant of the FWO Vlaanderen, the IAP P7/08 CHARM (Belspo) and the GOA-2015-014 (KU Leuven) (TVD); Program No 9 of the Presidium of the Russian Academy of Sciences (DYK).

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Correspondence to V. M. Nakariakov.

Appendix

Appendix

Abbreviations and acronyms commonly used in solar coronal and Earth’s magnetospheric physics:

AAR:

Auroral acceleration region

AIA:

Atmospheric Imaging Assembly on SDO

BBF:

bursty bulk flow events

CBF:

coronal bright fronts

CIR:

Corotating interaction region

CME:

Coronal mass ejection

CSHKP:

Carmichael, Sturrock, Hirayama, Kopp-Pneuman (or standard) model of a solar flare

EIS:

Extreme Ultraviolet Imaging Spectrometer on Hinode

EIT:

Extreme Ultraviolet Imaging Telescope on SoHO

EMIC:

Electromagnetic ion-cyclotron

EUV:

Extreme Ultraviolet

FLR:

field line resonance—an eigenmode of a closed geomagnetic field line

FMS:

Fast magnetosonic

FTE:

Flux transfer events

IAR:

Ionospheric Alfvénic resonator

IMF:

Interplanetary magnetic field

IRI:

International Reference Ionosphere model

KAWs:

Kinetic Alfvén waves

KHI:

Kelvin–Helmholtz instability

LLBL:

Low latitude boundary layer

LoS:

Line-of-sight

MHD:

Magnetohydrodynamic

MP:

Magnetopause

MSIS:

Mass Spectrometer—Incoherent Scatter Model of the upper atmosphere

NFTE:

Nightside flux transfer events

NoRH:

Nobeyama Radioheliograph

NRH:

Nancey RadioHeliograph

QPPs:

Quasi-periodic pulsations

RHESSI:

Reuven Ramaty High-Energy Solar Spectroscopic Imager

SDO:

NASA Solar Dynamics Observatory

SFE:

Solar flare effect

SI:

Sudden impulse

SID:

Sudden ionospheric disturbance

SoHO:

ESA/NASA Solar and Heliospheric Observatory

SSC:

Storm sudden commencement

SSRT:

Siberian Solar Radio Telescope

STEREO:

Solar TErrestrial RElations Observatory

SUMER:

Solar Ultraviolet Measurements of Emitted Radiation instrument on SOHO

SXT:

Solar X-ray Telescope on Yohkoh

TRACE:

Transition Region and Coronal Explorer

ULF:

Ultra low frequency

XRT:

X-ray Telescope on Hinode.

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Nakariakov, V.M., Pilipenko, V., Heilig, B. et al. Magnetohydrodynamic Oscillations in the Solar Corona and Earth’s Magnetosphere: Towards Consolidated Understanding. Space Sci Rev 200, 75–203 (2016). https://doi.org/10.1007/s11214-015-0233-0

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  • DOI: https://doi.org/10.1007/s11214-015-0233-0

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