Journal Article

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

Tsuzuki, Toshihiro, Feller, Alex, Harnes, Edvarda, Bernasconi, Pietro, Bell, Alexander, Tamura, Tomonori, Carpenter, Michael, Strecker, Hanna, Naito, Yoshihiro, Raouafi, Nour E, Grauf, Bianca, Oba, Takayoshi, Vukadinović, Dušan, Matsumoto, Takuma, Álvarez-Herrero, Alberto, Martínez Pillet, Valentín, Lagg, Andreas, Gandorfer, Achim, Katsukawa, Yukio, Suematsu, Yoshinori, Quintero Noda, Carlos, Shinoda, Kazuya, Kawabata, Yusuke, Ishikawa, Ryohtaroh T, Blanco Rodríguez, Julian, Hara, Hirohisa, Orozco Suárez, David, Smitha, H. N, Solanki, Sami K, Berkefeld, Thomas, Riethmüller, Tino L, Bailén, Francisco Javier, Castellanos Durán, Juan Sebastián, Siu-Tapia, Azaymi L, Santamarina Guerrero, Pablo, Kubo, Masahito, Uraguchi, Fumihiro, del Toro Iniesta, Jose Carlos, Shimizu, Toshifumi, Hölken, Johannes, Iglesias, Francisco A

2026

Overview

We report high-spatial-resolution spectropolarimetric observations spatially associated with a solar filament, obtained with the Sunrise Chromospheric Infrared Spectro-Polarimeter (SCIP) on board the Sunrise iii balloon-borne solar observatory on 2024 July 15. The observed filament was located near the solar disk center, adjacent to an active region, and remained quiescent for at least 2 hr 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 2σ 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 to the vector magnetic structure of solar filaments in the lower chromosphere, complementing existing He i based diagnostics that probe the upper chromosphere.

• Publisher: IOP Publishing
• Subject: Chromosphere / Field of view / Field strength / Filaments / Linear polarization / Magnetic fields / Magnetic properties / Magnetic structure / Noise levels / Polarimeters / Polarization / Solar filaments / Solar observatories / Vectors (mathematics) / Zeeman effect