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Alfvén-magnetosonic waves interaction in the solar corona

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Abstract

The nonlinear propagation of the Alfvén and magnetosonic waves in the solar corona is investigated in terms of model equations. Due to viscous effects taken into account the propagation of the fast wave itself is governed by Burgers type equations possessing both expansion and compression shock solutions. Numerical simulations show that both parallely and perpendicularly propagating fast waves can steepen into shocks if their amplitudes are in excess of some sizeable fraction of the Alfvén velocity. However, if the magnetic field changes linearly in the perpendicular direction, then formation of perpendicular shocks can be hindered. The Alfvén waves exhibit a tendency to drive both the slow and fast magnetosonic waves whose propagation is described by linearized Boussinesq type equations with ponderomotive terms due to the Alfvén wave. The limits of the slow and fast waves are investigated.

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Authors and Affiliations

  1. Department of Mathematical Sciences, The Mathematical Institute, University of St Andrews, KY16 9SS, St Andrews, Scotland

    K. Murawski

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  1. K. Murawski
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Murawski, K. Alfvén-magnetosonic waves interaction in the solar corona. Sol Phys 139, 279–297 (1992). https://doi.org/10.1007/BF00159155

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  • DOI: https://doi.org/10.1007/BF00159155

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