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Synthetic Radio Views of Simulated Solar Flux Ropes

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Abstract

We produce synthetic radio views of simulated flux ropes in the solar corona, where finite-\(\upbeta\) magnetohydrodynamic (MHD) simulations serve to mimic the flux-rope formation stages, as well as their stable endstates. These endstates represent twisted flux ropes where balancing Lorentz forces, gravity, and pressure gradients determine the full thermodynamic variation throughout the flux rope. The models obtained are needed to quantify radiative transfer in radio bands, and they allow us to contrast weak with strong magnetic-field conditions. Field strengths of up to 100 G in the flux rope yield radio views dominated by optically thin free–free emission. The forming flux rope shows clear morphological changes in its emission structure as it deforms from an arcade to a flux rope, both on disk and at the limb. For an active-region filament channel with a field strength of up to 680 G in the flux rope, gyroresonance emission (from the third and fourth gyrolayers) can be detected, and it even dominates free–free emission at frequencies of up to 7 GHz. Finally, we also show synthetic views of a simulated filament embedded within a (weak-field) flux rope, resulting from an energetically consistent MHD simulation. For this filament, synthetic views at the limb show clear similarities with actual observations, and the transition from optically thick (below 10 GHz) to optically thin emission can be reproduced. On the disk, its dimension and temperature conditions are as yet not realistic enough to yield the observed radio-brightness depressions.

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Notes

  1. More exactly, the cutoff frequency of the extraordinary mode slightly exceeds the plasma frequency. However, under the considered conditions this difference is negligible.

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Acknowledgments

This work was supported in part by the Russian Foundation of Basic Research (grants 14-02-91157 and 15-02-03717) and by a Marie Curie International Research Staff Exchange Scheme “Radiosun” (PEOPLE-2011-IRSES-295272). R. Keppens and C. Xia acknowledge support from the project GOA/2015/014 (KU Leuven), the Interuniversity Attraction Poles Programme initiated by the Belgian Science Policy Office (IAP P7/08 CHARM), and the FWO. Part of the simulations used the VSC (Flemish Supercomputer Center) funded by the Hercules foundation and the Flemish Government.

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  1. Institute of Solar-Terrestrial Physics, Irkutsk, 664033, Russia

    A. A. Kuznetsov

  2. CmPA, Department of Mathematics, KU Leuven, 3001, Leuven, Belgium

    R. Keppens & C. Xia

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Kuznetsov, A.A., Keppens, R. & Xia, C. Synthetic Radio Views of Simulated Solar Flux Ropes. Sol Phys 291, 823–845 (2016). https://doi.org/10.1007/s11207-016-0865-6

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