Energy transport and heating by torsional Alfvén waves propagating from the photosphere to the corona in the quiet Sun

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dc.contributor.author Soler, R.
dc.contributor.author Terradas, J.
dc.contributor.author Oliver, R.
dc.contributor.author Ballester, J.L.
dc.date.accessioned 2023-12-21T11:42:38Z
dc.date.available 2023-12-21T11:42:38Z
dc.identifier.uri http://hdl.handle.net/11201/163320
dc.description.abstract [eng] In the solar atmosphere, Alfvén waves are believed to play an important role in the transfer of energy from the photosphere to the corona and solar wind, and in the heating of the chromosphere. We perform numerical computations to investigate the energy transport and dissipation associated with torsional Alfvén waves propagating in magnetic flux tubes that expand from the photosphere to the corona in quiet-Sun conditions. We place a broadband driver at the photosphere that injects a wave energy flux of 107 erg cm−2 s−1 and consider Ohm's magnetic diffusion and ion-neutral collisions as dissipation mechanisms. We find that only a small fraction of the driven flux, ∼105 erg cm−2 s−1, is able to reach coronal heights, but it may be sufficient to partly compensate the total coronal energy loss. The frequency of maximal transmittance is ∼5 mHz for a photospheric field strength of 1 kG and is shifted to smaller/larger frequencies for weaker/stronger fields. Lower frequencies are reflected at the transition region, while higher frequencies are dissipated, producing enough heat to balance chromospheric radiative losses. Heating in the low and middle chromosphere is due to Ohmic dissipation, while ion-neutral friction dominates in the high chromosphere. Ohmic diffusion is enhanced by phase mixing because of the expansion of the magnetic field. This effect has the important consequence of increasing the chromospheric dissipation and, therefore, reducing the energy flux that reaches the corona. We provide empirical fits of the transmission coefficient that could be used as input for coronal models.
dc.format application/pdf
dc.relation.isformatof Reproducció del document publicat a: https://doi.org/10.3847/1538-4357/aaf64c
dc.relation.ispartof The Astrophysical Journal, 2019, vol. 871, num. 3, p. 1-19
dc.rights (c) American Astronomical Society, 2019
dc.subject.classification 53 - Física
dc.subject.other 53 - Physics
dc.title Energy transport and heating by torsional Alfvén waves propagating from the photosphere to the corona in the quiet Sun
dc.type info:eu-repo/semantics/article
dc.type info:eu-repo/semantics/publishedVersion
dc.date.updated 2023-12-21T11:42:38Z
dc.subject.keywords magnetohydrodynamics
dc.subject.keywords Sun: atmosphere
dc.subject.keywords Sun: oscillations
dc.rights.accessRights info:eu-repo/semantics/openAccess
dc.identifier.doi https://doi.org/10.3847/1538-4357/aaf64c


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