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Delayed, Line-dependent Reorganization of Pore Oscillations Following a Compact C8.2 Flare Observed by SUNRISE III/SUSI

  • Authors: Shahin Jafarzadeh, David B. Jess, Marco Stangalini, Lyndsay Fletcher, Ryan O. Milligan, Paulo J. A. Simões, Peter H. Keys, Sami K. Solanki, H. N. Smitha, Andreas Lagg, Achim Gandorfer, Alex Feller, Francisco A. Iglesias, Tino L. Riethmüller, Bianca Grauf, Johannes Hoelken, Jose Carlos del Toro Iniesta, Yukio Katsukawa, Pietro Bernasconi, Thomas Berkefeld, Alberto Álvarez-Herrero, Masahito Kubo, David Orozco Suárez, Michael Carpenter, Alexander Bell, Valentín Martínez Pillet, Francisco Javier Bailén, Julian Blanco Rodríguez, Juan Sebastián Castellanos Durán, Edvarda Harnes, Ryohtaroh T. Ishikawa, Yusuke Kawabata, Takuma Matsumoto, Takayoshi Oba, Azaymi L. Siu-Tapia, Hanna Strecker, Dušan Vukadinović

Shahin Jafarzadeh et al 2026 The Astrophysical Journal Letters 1010 .

  • Provider: AAS Journals

Caption: Figure 4.

RGWS power relative to the preevent interval. The spectral lines are ordered by their line-core enhancement at the flare peak. Panels (a) and (b) show the 4.2–7.0 and 7.0–11.5 mHz bands, respectively. Open blue circles denote the early postevent ratio, and filled red circles denote the late postevent ratio; gray connectors show the change between these intervals. Horizontal bars give paired 95% bootstrap confidence intervals for the ratios of the spatially averaged band powers, obtained by resampling spatial blocks. The vertical line at unity denotes no change from the preevent state.

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