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Evidence of ubiquitous Alfvén pulses transporting energy from the photosphere to the upper chromosphere

The multi-million degree temperature increase from the middle to the upper solar atmosphere is one of the most fascinating puzzles in plasma-astrophysics. Although magnetic waves might transport enough energy from the photosphere to heat up the local chromosphere and corona, observationally validati...

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Detalles Bibliográficos
Autores principales: Liu, Jiajia, Nelson, Chris J., Snow, Ben, Wang, Yuming, Erdélyi, Robert
Formato: Online Artículo Texto
Lenguaje:English
Publicado: Nature Publishing Group UK 2019
Materias:
Acceso en línea:https://www.ncbi.nlm.nih.gov/pmc/articles/PMC6683129/
https://www.ncbi.nlm.nih.gov/pubmed/31383869
http://dx.doi.org/10.1038/s41467-019-11495-0
Descripción
Sumario:The multi-million degree temperature increase from the middle to the upper solar atmosphere is one of the most fascinating puzzles in plasma-astrophysics. Although magnetic waves might transport enough energy from the photosphere to heat up the local chromosphere and corona, observationally validating their ubiquity has proved challenging. Here, we show observational evidence that ubiquitous Alfvén pulses are excited by prevalent intensity swirls in the solar photosphere. Correlation analysis between swirls detected at different heights in the solar atmosphere, together with realistic numerical simulations, show that these Alfvén pulses propagate upwards and reach chromospheric layers. We found that Alfvén pulses carry sufficient energy flux (1.9 to 7.7 kW m(−2)) to balance the local upper chromospheric energy losses (~0.1 kW m(−2)) in quiet regions. Whether this wave energy flux is actually dissipated in the chromosphere and can lead to heating that balances the losses is still an open question.