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Formation of Coronal Large-Amplitude Waves and the Chromospheric Response

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Abstract

An in-depth analysis of numerical simulations is performed to obtain a deeper insight into the nature of various phenomena occurring in the solar atmosphere as a consequence of the eruption of unstable coronal structures. Although the simulations take into account only the most basic characteristics of a flux-rope eruption, the simulation analysis reveals important information on various eruption-related effects. It quantifies the relation between the eruption dynamics and the evolution of the large-amplitude coronal magnetohydrodynamic wave and the associated chromospheric downward-propagating perturbation. We show that the downward propagation of the chromospheric Moreton-wave disturbance can be approximated by a constant-amplitude switch-on shock that moves through a medium of rapidly decreasing Alfvén velocity. The presented analysis reveals the nature of secondary effects that are observed as coronal upflows, secondary shocks, various forms of wave-trains, delayed large-amplitude slow disturbances, transient coronal depletions, etc. We also show that the eruption can cause an observable Moreton wave and a secondary coronal front only if it is powerful enough and is preferably characterized by significant lateral expansion. In weaker eruptions, only the coronal and transition-region signatures of primary waves are expected to be observed. In powerful events, the primary wave moves at an Alfvén Mach number significantly larger than 1 and steepens into a shock that is due to the nonlinear evolution of the wavefront. After the eruption-driven phase, the perturbation evolves as a freely propagating simple wave, characterized by a significant deceleration, amplitude decrease, and wave-profile broadening. In weak events the coronal wave does not develop into a shock and propagates at a speed close to the ambient magnetosonic speed.

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Acknowledgements

This work has been supported by Croatian Science Foundation under the project 6212 “Solar and Stellar Variability” and the European Commission’s Seventh Framework Programme (FP7/2007-2013) projects under the grant agreement No. 263252 (project COMESEP, www.comesep.eu ) and No. 284461 (project eHEROES, soteria-space.eu/eheroes/html/ ). M.T. and A.M.V. acknowledge the Austrian Science Fund (FWF): FWF V195-N16 and P24092-N16. The Versatile Advection Code (VAC) was developed by Gábor Tóth at the Astronomical Institute at Utrecht. The project is a collaboration with the FOM Institute for Plasma Physics, the Mathematics department at Utrecht and the CWI at Amsterdam. In particular, Rony Keppens (FOM), Mikhail Botchev (Mathematics Dept.), and Auke van der Ploeg (CWI) contributed significantly to the development of the code. G. Tóth and R. Keppens share the responsibility and work associated with the development, maintenance, distribution, and management of the software. We are grateful to Tayeb Aiouaz and Tibor Török for help in getting acquainted with VAC. B.V. and A.M.V. thank ISSI (International Space Science Institute, Bern) for the hospitality provided to the team “The Nature of Coronal Bright Fronts” led by D. Long and S. Bloomfield, where many of the ideas presented in this work have been discussed.

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Authors and Affiliations

  1. Hvar Observatory, Faculty of Geodesy, University of Zagreb, Kačićeva 26, 10000, Zagreb, Croatia

    B. Vršnak & T. Žic

  2. Karlovac University of Applied Sciences, Trg J.J. Strossmayera 9, 47000, Karlovac, Croatia

    S. Lulić

  3. IGAM, Institute of Physics, University of Graz, Universitätsplatz 5, 8010, Graz, Austria

    M. Temmer & A. M. Veronig

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  1. B. Vršnak
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Vršnak, B., Žic, T., Lulić, S. et al. Formation of Coronal Large-Amplitude Waves and the Chromospheric Response. Sol Phys 291, 89–115 (2016). https://doi.org/10.1007/s11207-015-0822-9

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