Magnetic tornadoes as energy channels into the solar corona

Sven Wedemeyer-Böhm*, Eamon Scullion, Oskar Steiner, Luc Rouppe Van Der Voort, Jaime De La Cruz Rodriguez, Viktor Fedun, Robert Erdélyi

*Corresponding author for this work

Research output: Contribution to journalLetterpeer-review

259 Citations (Scopus)


Heating the outer layers of the magnetically quiet solar atmosphere to more than one million kelvin and accelerating the solar wind requires an energy flux of approximately 100 to 300watts per square metre, but how this energy is transferred and dissipated there is a puzzle and several alternative solutions have been proposed. Braiding and twisting of magnetic field structures, which is caused by the convective flows at the solar surface, was suggested as an efficient mechanism for atmospheric heating. Convectively driven vortex flows that harbour magnetic fields are observed to be abundant in the photosphere (the visible surface of the Sun). Recently, corresponding swirling motions have been discovered in the chromosphere, the atmospheric layer sandwiched between the photosphere and the corona. Here we report the imprints of these chromospheric swirls in the transition region and low corona, and identify them as observational signatures of rapidly rotating magnetic structures. These ubiquitous structures, which resemble super-tornadoes under solar conditions, reach from the convection zone into the upper solar atmosphere and provide an alternative mechanism for channelling energy from the lower into the upper solar atmosphere.

Original languageEnglish
Pages (from-to)505-508
Number of pages4
Issue number7404
Publication statusPublished - 28 Jun 2012


Dive into the research topics of 'Magnetic tornadoes as energy channels into the solar corona'. Together they form a unique fingerprint.

Cite this