Chromospheric Alfvénic Waves Strong Enough to Power the Solar Wind
B. De Pontieu, S. W. McIntosh, M. Carlsson, V. H. Hansteen, T. D. Tarbell, C. J.
Schrijver, A. M. Title, R. A. Shine, S. Tsuneta, Y. Katsukawa, K. Ichimoto, Y. Suematsu,
T. Shimizu, S. Nagata
Supporting Online Material
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Materials and Methods
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Figs. S1 to S6
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Movies S1 and S5
Movie S1.
Movie illustrating the temporal evolution of the spicule shown in Fig. 1 as imaged by Hinode SOT in Ca II H 3968 Å filtergrams. This movie has the original orientation of the data, so it is rotated with respect to Fig. 1.
Movie S2.
Movie illustrating the temporal evolution of spicules shown in Fig. 2A as imaged by Hinode SOT in Ca II H 3968 Å filtergrams, after unsharp masking to enhance features with spatial scales of order 150-200 km. Close to the limb the short-lived nature of the spicules is very apparent, whereas higher up significant swaying can be observed that is caused by Alfvén waves.
Movie S3.
Movie illustrating the temporal evolution of the spicule described in the xt cuts of fig. S6. Unsharp masked images reveal the rotation the spicule undergoes as it forms.
Movie S4.
Movie illustrating the temporal evolution of a simulated spicule forming while carrying a superposition of two Alfvén waves propagating in opposite directions, as described in the caption of fig. S6.
Movie S5.
Movie showing the shaking of the magnetic field in numerical simulations described in the text. For details on coloring, see caption of Fig. 4.
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