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Testing Alfvén wave propagation in a “realistic” set-up of the solar atmosphere

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dc.contributor.author Chatterjee, Piyali
dc.date.accessioned 2020-11-26T15:45:09Z
dc.date.available 2020-11-26T15:45:09Z
dc.date.issued 2020-07
dc.identifier.citation Geophysical & Astrophysical Fluid Dynamics, Vol.114, No.1–2, 213–234 en_US
dc.identifier.issn 0309-1929
dc.identifier.uri http://prints.iiap.res.in/handle/2248/7416
dc.description Restricted Access en_US
dc.description.abstract We present a radiative magneto-hydrodynamic simulation set-up using the pencil code to study the generation, propagation and dis- sipation of Alfvén waves in the solar atmosphere which includes a convective layer, photosphere below and chromosphere, transition region and the corona above. We prepare a set-up of steady-state solar convection where the imposed external magnetic field also has reached the final value gradually starting from a very small value. From that state, we start several simulations by varying the magnetic Prandtl number and the forcing strengths. We find the propaga- tion characteristics of waves excited in this simulation run depend strongly on the magnetic Prandtl number and the wave number of the forcing. For magnetic Prandtl number of unity, we obtain localised heating in the corona due to shock dissipation. en_US
dc.language.iso en en_US
dc.publisher Taylor & Francis en_US
dc.relation.uri https://doi.org/10.1080/03091929.2019.1672676
dc.rights © Taylor & Francis
dc.title Testing Alfvén wave propagation in a “realistic” set-up of the solar atmosphere en_US
dc.type Article en_US


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