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Coronal Shock Waves, EUV Waves, and Their Relation to CMEs. II. Modeling MHD Shock Wave Propagation Along the Solar Surface, Using Nonlinear Geometrical Acoustics

  • Energy Storage and Release – Models Meet Radio Observations
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Abstract

We model the propagation of a coronal shock wave, using nonlinear geometrical acoustics. The method is based on the Wentzel–Kramers–Brillouin (WKB) approach and takes into account the main properties of nonlinear waves: i) dependence of the wave front velocity on the wave amplitude, ii) nonlinear dissipation of the wave energy, and iii) progressive increase in the duration of solitary shock waves. We address the method in detail and present results of the modeling of the propagation of shock-associated extreme-ultraviolet (EUV) waves as well as Moreton waves along the solar surface in the simplest solar corona model. The calculations reveal deceleration and lengthening of the waves. In contrast, waves considered in the linear approximation keep their length unchanged and slightly accelerate.

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Authors and Affiliations

  1. Institute of Solar-Terrestrial Physics SB RAS, P.O. Box 291, Lermontov St. 126A, Irkutsk, 664033, Russia

    A. N. Afanasyev & A. M. Uralov

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  1. A. N. Afanasyev
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  2. A. M. Uralov
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Correspondence to A. N. Afanasyev.

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Energy Storage and Relase through the Solar Activity Cycle – Models Meet Radio Observations

Guest Editors: Christophe Marqué and Alexander Nindos.

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Afanasyev, A.N., Uralov, A.M. Coronal Shock Waves, EUV Waves, and Their Relation to CMEs. II. Modeling MHD Shock Wave Propagation Along the Solar Surface, Using Nonlinear Geometrical Acoustics. Sol Phys 273, 479–491 (2011). https://doi.org/10.1007/s11207-011-9730-9

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  • DOI: https://doi.org/10.1007/s11207-011-9730-9

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