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Expanding Magnetic Canopy Structure and Parasitic Polarities in a Quiet-Sun Network Element Observed by SUNRISE III/SCIP

Authors: Ryan J. Campbell, Carlos Quintero Noda, Mihalis Mathioudakis, Manuel Collados, Jack McFall, David B. Jess, 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, H. N. Smitha, David Orozco Suárez, Bianca Grauf, Michael Carpenter, Alexander Bell, Valentín Martínez Pillet, Francisco Javier Bailén, Julian Blanco Rodríguez, Juan Sebastián Castellanos Durán, Edvarda Harnes, Johannes Hölken, Francisco A. Iglesias, Ryohtaroh T. Ishikawa, Yusuke Kawabata, Takuma Matsumoto, Takayoshi Oba, Azaymi L. Siu-Tapia, Hanna Strecker, Dušan Vukadinović, Hirohisa Hara, Toshifumi Shimizu

Ryan J. Campbell et al 2026 The Astrophysical Journal Letters 1008 .

Provider: AAS Journals

Caption: Figure 6.

Example Stokes profile and inversion fits for the location marked by the star in Figure 4. Observed (dashed) and fitted (solid) Stokes profiles are shown for Fe I 8468 Å, Ca II 8498 Å, Fe I 8514 Å, Fe I 8515 Å, and Ca II 8542 Å. The Stokes V profiles exhibit opposite polarity between the photospheric Fe lines and the chromospheric Ca lines. The lower panels (bottom row) show the inferred atmospheric stratification as a function of optical depth, including the temperature, magnetic field strength, LOS velocity, magnetic inclination, and magnetic azimuth returned by the inversion.

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