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Chromospheric Dynamics of an Umbral Flare Kernel—Based on Coordinated SUNRISE III SCIP and Domeless Solar Telescope Observations

  • Authors: Ayumi Asai, Satoru UeNo, Takuma Matsumoto, Takayoshi Oba, Yukio Katsukawa, Masahito Kubo, Ryohtaroh T. Ishikawa, Yusuke Kawabata, Hirohisa Hara, Yoshihiro Naito, Toshifumi Shimizu, Sami K. Solanki, Andreas Lagg, Achim Gandorfer, Jose Carlos del Toro Iniesta, Pietro Bernasconi, Thomas Berkefeld, Alex Feller, Tino L. Riethmüller, Alberto Álvarez-Herrero, H. N. Smitha, David Orozco Suárez, Bianca Grauf, Michael Carpenter, Alexander Bell, Valentín Martínez Pillet, Laurent Gizon, Francisco Javier Bailén, Julian Blanco Rodríguez, Juan Sebastián Castellanos Durán, Edvarda Harnes, Johannes Hoelken, Francisco A. Iglesias, Azaymi L. Siu-Tapia, Hanna Strecker, Dušan Vukadinović

Ayumi Asai et al 2026 The Astrophysical Journal Letters 1008 .

  • Provider: AAS Journals

Caption: Figure 5.

(a) Ca 8542 line-center image of the flare kernel at 03:04:15 UT observed with SCIP. Colored symbols indicate the locations within the flare kernel from which the spectra shown in panel (b) were extracted. The asterisks ∗ are located along the left thread, while the diamonds ⋄ mark the right thread. The triangle △ indicates a nearby reference point in the umbra (outside the kernel). (b) Ca 8542 spectra obtained at the positions along the left thread indicated by the asterisk ∗ in panel (a). Solid and dashed curves represent spectra at 03:04:15 and 03:10:15 UT, respectively. (c) Same as panel (a), but for observations at 03:10:15 UT. (d) Same as panel (b), but for the right thread. In panels (b) and (d), all spectra are normalized to the local continuum level. The spectra at the reference point indicated by triangle △ in panels (a) and (c) are shown in gray. The other spectra are shown as difference spectra relative to the reference point. The time shown for each raster image or spectrum indicates the start time of the corresponding raster scan.

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