Torsional oscillations within a magnetic pore in the solar photosphere

Authors Organisations
  • Marco Stangalini(Author)
    Italian Space Agency
  • Robertus Erdélyi(Author)
    The University of Sheffield
    Eötvös L. University
    Hungarian Solar Physics Foundation (HSPF)
  • Callum Boocock(Author)
    Queen Mary University of London
  • David Tsiklauri(Author)
    Queen Mary University of London
  • Christopher J. Nelson(Author)
    Queen's University Belfast
  • Dario Del Moro(Author)
    University of Rome Tor Vergata
  • Francesco Berrilli(Author)
    University of Rome Tor Vergata
  • Marianna B. Korsós(Author)
    The University of Sheffield
    Eötvös L. University
Type Article
Original languageEnglish
Pages (from-to)691-696
Number of pages6
JournalNature Astronomy
Issue number7
Early online date10 May 2021
Publication statusPublished - 01 Jul 2021
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Alfvén waves have proven to be important in a range of physical systems due to their ability to transport non-thermal energy over long distances in a magnetized plasma. This property is of specific interest in solar physics, where the extreme heating of the atmosphere of the Sun remains unexplained. In an inhomogeneous plasma such as a flux tube in the solar atmosphere, they manifest as incompressible torsional perturbations. However, despite evidence in the upper atmosphere, they have not been directly observed in the photosphere. Here, we report the detection of antiphase incompressible torsional oscillations observed in a magnetic pore in the photosphere by the Interferometric Bidimensional Spectropolarimeter. State-of-the-art numerical simulations suggest that a kink mode is a possible excitation mechanism of these waves. The excitation of torsional waves in photospheric magnetic structures can substantially contribute to the energy transport in the solar atmosphere and the acceleration of the solar wind, especially if such signatures will be ubiquitously detected in even smaller structures with the forthcoming next generation of solar telescopes.