MHD Wave Modes Resolved in Fine-Scale Chromospheric Magnetic Structures

G. Verth, D. B. Jess

Research output: Chapter in Book/Report/Conference proceedingChapter

10 Citations (Scopus)
289 Downloads (Pure)


Due to its complex and dynamic fine-scale structure, the chromosphere is a particularly challenging region of the Sun's atmosphere to understand. It is now widely accepted that to model chromospheric dynamics, even on a magnetohydrodynamic (MHD) scale, while also calculating spectral line emission, one must realistically include the effects of partial ionization and radiative transfer in a multi-fluid plasma under non-LTE conditions. Accurate quantification of MHD wave energetics must befounded on a precise identification of the actual wave mode being observed. This chapter focuses on MHD kink-mode identification, MHD sausage mode identification, and MHD torsional Alfvén wave identification. It then reviews progress in determining more accurate energy flux estimations of specific MHD wave modes observed in the chromosphere. The chapter finally examines how the discovery of these MHD wave modes has helped us advance the field of chromosphericmagnetoseismology.
Original languageEnglish
Title of host publicationLow-Frequency Waves in Space Plasmas
EditorsAndreas Keiling, Dong-Hun Lee, Valery Nakariakov
PublisherJohn Wiley & Sons Inc.
Number of pages16
ISBN (Electronic)9781119055006
ISBN (Print)9781119054955
Publication statusPublished - 12 Feb 2016

Publication series

NameGeophysical Monograph Series
ISSN (Print)0065-8448


Dive into the research topics of 'MHD Wave Modes Resolved in Fine-Scale Chromospheric Magnetic Structures'. Together they form a unique fingerprint.

Cite this