Vector Magnetic Field associated with an Active Region Filament Observed by SUNRISE III/SCIP in the Ca II 8542 Å Line

Takuma Matsumoto; Yukio Katsukawa; Masahito Kubo; Yusuke Kawabata; Takayoshi Oba; Ryohtaroh T. Ishikawa; Yoshihiro Naito; Hirohisa Hara; Toshifumi Shimizu; Fumihiro Uraguchi; Toshihiro Tsuduki; Kazuya Shinoda; Tomonori Tamura; Yoshinori Suematsu; Carlos Quintero Noda; 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; Francisco Javier Bailén; Julian Blanco Rodríguez; Juan Sebastián Castellanos Durán; Edvarda Harnes; Johannes Hölken; Francisco A. Iglesias; Azaymi L. Siu Tapia; Hanna Strecker; Dušan Vukadinović; Pablo Santamarina Guerrero; Nour E. Raouafi

arXiv · 2606.16088

Vector Magnetic Field associated with an Active Region Filament Observed by SUNRISE III/SCIP in the Ca II 8542 Å Line

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Abstract

We report high-spatial-resolution spectropolarimetric observations spatially associated with a solar filament, obtained with the SUNRISE Chromospheric Infrared spectro-Polarimeter (SCIP) onboard the SUNRISE III balloon-borne solar observatory on 15 July 2024. The observed filament was located near the solar disk center, adjacent to an active region, and remained quiescent for at least two hours during the observing period. SCIP recorded full Stokes profiles in the Ca II 8542 Å line, revealing clear signatures of linear polarization produced by the transverse Zeeman effect. The detected linear polarization signals within the filament region exceeded the 2$σ$ noise level and exhibited a characteristic Zeeman double-lobe spectral shape that distinguishes them from polarization due to scattering. The magnetic field strength derived using the weak field approximation is approximately -80 G along the line of sight and 300-500 G in the transverse direction. These values likely reflect the magnetic properties of the filament and its supporting chromospheric environment. The orientation of the magnetic field vector is nearly parallel to the filament axis in its northeastern portion, while the southeastern part of the filament extends outside the field of view. To our knowledge, this is the first unambiguous detection of linear polarization associated with a solar filament with the Ca II 8542 Å line. Our results open a new diagnostic window on the vector magnetic structure of solar filaments in the lower chromosphere, complementing existing He I based diagnostics that probe the upper chromosphere.

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Takuma Matsumoto, Yukio Katsukawa, Masahito Kubo, Yusuke Kawabata, Takayoshi Oba, Ryohtaroh T. Ishikawa, Yoshihiro Naito, Hirohisa Hara, Toshifumi Shimizu, Fumihiro Uraguchi, Toshihiro Tsuduki, Kazuya Shinoda, Tomonori Tamura, Yoshinori Suematsu, Carlos Quintero Noda, 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, Francisco Javier Bailén, Julian Blanco Rodríguez, Juan Sebastián Castellanos Durán, Edvarda Harnes, Johannes Hölken, Francisco A. Iglesias, Azaymi L. Siu Tapia, Hanna Strecker, Dušan Vukadinović, Pablo Santamarina Guerrero, Nour E. Raouafi. 2026-06-15. Vector Magnetic Field associated with an Active Region Filament Observed by SUNRISE III/SCIP in the Ca II 8542 Å Line. https://arxiv.org/abs/2606.16088

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