Waves in Solar Coronal Loops
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TLDR
In this paper, the authors present recent progress in the observational study of four types of wave (or oscillation) phenomena mainly occurring in active region coronal loops, including (i) flare-induced slow mode oscillations, (ii) fast kink mode oscillation, (iii) propagating slow magnetoacoustic waves, and (iv) ubiquitous propagating kink (Alfvenic) waves.Abstract:
Recent observations have revealed the ubiquitous presence of magnetohydrodynamic (MHD) waves and oscillations in the solar corona. The aim of this review is to present recent progress in the observational study of four types of wave (or oscillation) phenomena mainly occurring in active region coronal loops, including (i) flare-induced slow mode oscillations, (ii) fast kink mode oscillations, (iii) propagating slow magnetoacoustic waves, and (iv) ubiquitous propagating kink (Alfvenic) waves. This review not only comprehensively outlines various aspects of these waves and coronal seismology, but also highlights the topics that are newly emerging or hotly debated, thus can provide readers a useful guidance on further studies of their interested topics.read more
Citations
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Alfven Waves in the Solar Corona
Steven Tomczyk,Scott W. McIntosh,Stephen L. Keil,Philip G. Judge,Thomas A. Schad,D. H. Seeley,J. Edmondson +6 more
TL;DR: An estimate of the energy carried by the waves that are spatially resolved indicates that they are too weak to heat the solar corona; however, unresolved Alfvén waves may carry sufficient energy.
Evolution of Magnetic Field and Energy in A Major Eruptive Active Region Based on SDO/HMI Observation
Xudong Sun,J. Todd Hoeksema,Yang Liu,Thomas Wiegelmann,Keiji Hayashi,Qingrong Chen,Julia K. Thalmann +6 more
TL;DR: In this paper, the authors report the evolution of magnetic field and its energy in NOAA active region 11158 over 5 days based on a vector magnetogram series from the Helioseismic and Magnetic Imager (HMI) on board the Solar Dynamic Observatory (SDO).
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Achievements of Hinode in the first eleven years
Khalid Al-Janabi,Patrick Antolin,Deborah Baker,Luis R. Bellot Rubio,Louisa Bradley,David H. Brooks,Rebecca Centeno,J. Leonard Culhane,Giulio Del Zanna,George A. Doschek,Lyndsay Fletcher,Hirohisa Hara,Louise K. Harra,Andrew Hillier,Andrew Hillier,Shinsuke Imada,James A. Klimchuk,John T. Mariska,Tiago M. D. Pereira,Katharine K. Reeves,Taro Sakao,Taro Sakao,Takashi Sakurai,Toshifumi Shimizu,Toshifumi Shimizu,Masumi Shimojo,Daikou Shiota,Daikou Shiota,Sami K. Solanki,Alphonse C. Sterling,Yingna Su,Yoshinori Suematsu,Theodore D. Tarbell,Sanjiv K. Tiwari,Shin Toriumi,Ignacio Ugarte-Urra,Harry P. Warren,Tetsuya Watanabe,Peter R. Young +38 more
TL;DR: In this article, an open access article distributed under the terms of the Creative Commons CC BY license, which permits unrestricted use, distribution, and reproduction in any medium, provided the original work is properly cited.
Coronal Plasma Motions near Footpoints of Active Region Loops Revealed from Spectroscopic Observations with {it Hinode} EIS
Hirohisa Hara,Tetsuya Watanabe,Louise K. Harra,J. Leonard Culhane,Peter R. Young,G. A. Doschek,John T. Mariska +6 more
TL;DR: In this article, the Hinode EUV Imaging Spectrometer was used to observe the solar active region 10938 from the disk center to the west limb with a single Gaussian approximation for the emission line profiles.
Full Sun Observations for Identifying the Source of the Slow Solar Wind.
TL;DR: This map provides a full-Sun observation that combines three key ingredients for identifying the sources: velocity, plasma composition and magnetic topology and shows them as solar wind composition plasma outflowing on open magnetic field lines.
References
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TRACE observation of damped coronal loop oscillations: implications for coronal heating
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On Solving the Coronal Heating Problem
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TL;DR: In this article, the authors investigated the nature of oscillations in a magnetic cylinder embedded in magnetic environment and showed that the standard slender flux tube analysis of a kink mode in a cylinder excludes the possibility of a second mode, which arises under photospheric conditions.
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Mass and Energy Flow in the Solar Chromosphere and Corona
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