English (United Kingdom)

https://curated-unify.zendy.io/wp-json/zendy-region/v1/featured_content/oa?rat=en

https://curated-unify.zendy.io/wp-json/zendy-region/v1/highlighted_journal/

Global: Zendy Plus annual

Presents the access of premium content as premium feature

Premium Content

Presents the keyphrase highlighting as premium feature

Keyphrase Highlighting

Presents the summarisation as premium feature

Summarisation

Insights

Presents the pdf analysis as premium feature

PDF Analysis

Presents the zaia usage as premium feature

ZAIA

Global: Zendy Tools annual

Global: Zendy Free Plan

Global: Zendy Tools monthly

Global: Zendy Plus monthly

The aim of this work is to study the energy transport by means of MHD wavespropagating in quiet Sun magnetic topology from layers below the surface to thecorona. Upward propagating waves find obstacles, such as the equipartitionlayer with plasma b=1 and the transition region, and get converted, reflectedand refracted. Understanding the mechanisms by which MHD waves can reach thecorona can give us information about the solar atmosphere and the magneticstructures. We carry out two-dimensional numerical simulations of wavepropagation in a magnetic field structure that consists of two vertical fluxtubes separated by an arcade shaped magnetic field. This configuration containsa null point in the corona, that significantly modifies the behaviour of thewaves. We describe in detail the wave propagation through the atmosphere underdifferent driving conditions. We also present the spatial distribution of themean acoustic and magnetic energy fluxes and the spatial distribution of thedominant frequencies in the whole domain. We conclude that the energy reachesthe corona preferably along vertical magnetic fields, inside the flux tubes,and it has an acoustic nature. Most of the magnetic energy keeps concentratedbelow the transition region due to the refraction of the magnetic waves and thecontinuous conversion of acoustic-like waves into fast magnetic waves in theequipartition layer located in the photosphere. However, part of the magneticenergy reaches the low corona when propagating in the region where the arcadesare located, but waves are sent back downwards to the lower atmosphere at thenull point surroundings. This phenomenon, together with the reflection andrefraction of waves in the TR and the lower turning point, act as a re-feedingof the atmosphere. In the frequency distribution, we find that high frequencywaves can reach the corona outside the vertical flux tubes.

MHD wave propagation from the sub-photosphere to the corona in an arcade-shaped magnetic field with a null point