Solar Physics

, Volume 246, Issue 1, pp 3–29

Present and Future Observing Trends in Atmospheric Magnetoseismology


DOI: 10.1007/s11207-007-9029-z

Cite this article as:
Banerjee, D., Erdélyi, R., Oliver, R. et al. Sol Phys (2007) 246: 3. doi:10.1007/s11207-007-9029-z


With modern imaging and spectral instruments observing in the visible, EUV, X-ray, and radio wavelengths, the detection of oscillations in the solar outer atmosphere has become a routine event. These oscillations are considered to be the signatures of a wave phenomenon and are generally interpreted in terms of magnetohydrodynamic (MHD) waves. With multiwavelength observations from ground- and space-based instruments, it has been possible to detect waves in a number of different wavelengths simultaneously and, consequently, to study their propagation properties. Observed MHD waves propagating from the lower solar atmosphere into the higher regions of the magnetized corona have the potential to provide excellent insight into the physical processes at work at the coupling point between these different regions of the Sun. High-resolution wave observations combined with forward MHD modeling can give an unprecedented insight into the connectivity of the magnetized solar atmosphere, which further provides us with a realistic chance to reconstruct the structure of the magnetic field in the solar atmosphere. This type of solar exploration has been termed atmospheric magnetoseismology. In this review we will summarize some new trends in the observational study of waves and oscillations, discussing their origin and their propagation through the atmosphere. In particular, we will focus on waves and oscillations in open magnetic structures (e.g., solar plumes) and closed magnetic structures (e.g., loops and prominences), where there have been a number of observational highlights in the past few years. Furthermore, we will address observations of waves in filament fibrils allied with a better characterization of their propagating and damping properties, the detection of prominence oscillations in UV lines, and the renewed interest in large-amplitude, quickly attenuated, prominence oscillations, caused by flare or explosive phenomena.


Coronal loopsMHD wavesMHD oscillations

Copyright information

© Springer Science+Business Media B.V. 2007

Authors and Affiliations

  • D. Banerjee
    • 1
  • R. Erdélyi
    • 2
  • R. Oliver
    • 3
  • E. O’Shea
    • 4
  1. 1.Indian Institute of AstrophysicsKoramangala, BangaloreIndia
  2. 2.Solar Physics and Space Plasma Research Centre (SP²RC), Department of MathematicsUniversity of SheffieldSheffieldEngland, UK
  3. 3.Departament de FísicaUniversitat de les Illes BalearsPalma de MallorcaSpain
  4. 4.Armagh ObservatoryCollege Hill, ArmaghNorthern Ireland, UK