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Observational Evidence of Vortex-driven Information Transfer in the Solar Atmosphere: Insights from SUNRISE III

  • Authors: Suzana S. A. Silva, Ioannis Dakanalis, Kostas Tziotziou, Azaymi L. Siu-Tapia, Shahin Jafarzadeh, Shivdev Singh Turkay, Viktor Fedun, Sami K. Solanki, Andreas Lagg, Achim Gandorfer, Jose Carlos del Toro Iniesta, Yukio Katsukawa, Pietro Bernasconi, Thomas Berkefeld, Alex Feller, Tino L. Riethmüller, Alberto Álvarez-Herrero, Masahito Kubo, Valentín Martínez Pillet, H. N. Smitha, David Orozco Suárez, Bianca Grauf, Michael Carpenter, Alexander Bell, Francisco Javier Bailén, Julian Blanco Rodríguez, Juan Sebastián Castellanos Durán, Edvarda Harnes, Johannes Hoelken, Francisco A. Iglesias, Ryohtaroh T. Ishikawa, Yusuke Kawabata, Takuma Matsumoto, Takayoshi Oba, Hanna Strecker, Dušan Vukadinovic, Maria Balaguer Jiménez, Esteban Sanchis Kilders, Ignacio Torralbo, Christoph Kuckein

Suzana S. A. Silva et al 2026 The Astrophysical Journal Letters 1008 .

  • Provider: AAS Journals

Caption: Figure 5.

Statistical comparison of GC between vortex regions and control regions for lag = 4.5 min. Left and middle panel: distributions of the peak mean GC per event for the two analyzed directions, wing→core (left) and core→wing (middle). Blue corresponds to vortices with lifetimes larger than 28 minutes (n = 20) and red to control regions (n = 782); dashed vertical lines indicate the respective sample means. Right panel: distribution of the directional asymmetry ﹩{\rm{\Delta }}{\rm{GC}}={\rm{GC}}({\rm{wing}}\to {\rm{core}})-{\rm{GC}}\,\,({\rm{core}}\to {\rm{wing}})﹩. ﹩{\rm{GC}}\,\,({\rm{wing}}\to {\rm{core}})﹩ quantifies the fraction of variance in the Mg I b2 core signal explained by past values of Mg I b2 wing signal, after accounting for the Mg I b2 signal’s own history, while ﹩{\rm{GC}}\,\,({\rm{core}}\to {\rm{wing}})﹩ represents the reverse coupling. Thus ΔGC measures the directional dominance of the interaction: positive values indicate comparatively stronger photosphere-to-chromosphere influence, whereas negative values indicate comparatively stronger chromosphere-to-photosphere influence.

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