Torsional oscillations within a magnetic pore in the solar photosphere

Marco Stangalini*, Robertus Erdélyi, Callum Boocock, David Tsiklauri, Christopher J. Nelson, Dario Del Moro, Francesco Berrilli, Marianna B. Korsós

*Awdur cyfatebol y gwaith hwn

Allbwn ymchwil: Cyfraniad at gyfnodolynErthygladolygiad gan gymheiriaid

20 Dyfyniadau (Scopus)
271 Wedi eu Llwytho i Lawr (Pure)

Crynodeb

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.
Iaith wreiddiolSaesneg
Tudalennau (o-i)691-696
Nifer y tudalennau6
CyfnodolynNature Astronomy
Cyfrol5
Rhif cyhoeddi7
Dyddiad ar-lein cynnar10 Mai 2021
Dynodwyr Gwrthrych Digidol (DOIs)
StatwsCyhoeddwyd - 01 Gorff 2021

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