Determining the Magnetic Field in the Atmosphere of a Solar Active Region Observed by the CLASP2.1 Sounding Rocket Experiment

Abstract We determine magnetic fields from the photosphere to the upper chromosphere combining data from the Hinode satellite and the CLASP2.1 sounding rocket experiment. CLASP2.1 provided polarization profiles of the Mg ii h and k lines, as well as of the Mn i lines around 2800 Å, across various magnetic structures in an active region, containing a plage, a pore, and the edges of a sunspot penumbra. By applying the weak-field approximation to the circular polarization profiles of these spectral lines, we obtain a longitudinal magnetic field map at three different heights in the chromosphere (lower, middle, and upper). This is complemented by data from Hinode (photospheric magnetic field), the Interface Region Imaging Spectrograph, and the Solar Dynamics Observatory (high spatial resolution observations of the chromosphere and corona). We quantify the height expansion of the plage magnetic fields and find that the magnetic fields expand significantly in the middle chromosphere, shaping the moss observed above in the transition region and corona. We identified an area with polarity reversal at the upper chromosphere around the edge of the pore, suggesting the presence of a magnetic discontinuity in the upper chromosphere. Transient and recurrent jetlike events are observed in this region, likely driven by magnetic reconnection. Around the penumbral edge, we find large-scale magnetic fields corresponding to the superpenumbral fibrils seen in the upper chromosphere. In the superpenumbral fibrils, we find Zeeman-induced linear polarization signals, suggesting the presence of a significantly inclined magnetic field, as strong as 1000 G in the upper chromosphere.

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Publication Details

Journal
The Astrophysical Journal
Published
2025-09-09
DOI
https://doi.org/10.3847/1538-4357/aded0e
Citations
3
Primary Topic
Solar and Space Plasma Dynamics
Type
article
Field-Weighted Citation Impact
3.46

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article

Determining the Magnetic Field in the Atmosphere of a Solar Active Region Observed by the CLASP2.1 Sounding Rocket Experiment

David McKenzie, Amy R. Winebarger, Jiří Štěpán, Adam Kobelski et al.
3 citations
The Astrophysical Journal
Solar and Space Plasma Dynamics
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article

Determining the Magnetic Field in the Atmosphere of a Solar Active Region Observed by the CLASP2.1 Sounding Rocket Experiment

David McKenzie, Amy R. Winebarger, Jiří Štěpán, Adam Kobelski, Donguk Song, Christian Bethge, Luca Belluzzi, Taro Sakao, F. Auchère, Genevieve D. Vigil, Tanausú del Pino Alemán, J. Trujillo Bueno, R. Ishikawa, Takenori J. Okamoto, Ernest Alsina Ballester, Laurel Rachmeler, Ryouhei Kano, Bart De Pontieu, K. Kobayashi, Hao Li
article en
3 citations

Abstract

Abstract We determine magnetic fields from the photosphere to the upper chromosphere combining data from the Hinode satellite and the CLASP2.1 sounding rocket experiment. CLASP2.1 provided polarization profiles of the Mg ii h and k lines, as well as of the Mn i lines around 2800 Å, across various magnetic structures in an active region, containing a plage, a pore, and the edges of a sunspot penumbra. By applying the weak-field approximation to the circular polarization profiles of these spectral lines, we obtain a longitudinal magnetic field map at three different heights in the chromosphere (lower, middle, and upper). This is complemented by data from Hinode (photospheric magnetic field), the Interface Region Imaging Spectrograph, and the Solar Dynamics Observatory (high spatial resolution observations of the chromosphere and corona). We quantify the height expansion of the plage magnetic fields and find that the magnetic fields expand significantly in the middle chromosphere, shaping the moss observed above in the transition region and corona. We identified an area with polarity reversal at the upper chromosphere around the edge of the pore, suggesting the presence of a magnetic discontinuity in the upper chromosphere. Transient and recurrent jetlike events are observed in this region, likely driven by magnetic reconnection. Around the penumbral edge, we find large-scale magnetic fields corresponding to the superpenumbral fibrils seen in the upper chromosphere. In the superpenumbral fibrils, we find Zeeman-induced linear polarization signals, suggesting the presence of a significantly inclined magnetic field, as strong as 1000 G in the upper chromosphere.

The Astrophysical JournalVol. 990(2)
Lockheed Martin (United States) (US), Marshall Space Flight Center (US), National Oceanic and Atmospheric Administration (US), Consejo Superior de Investigaciones Científicas (ES), Universidad de La Laguna (ES), Cooperative Institute for Research in Environmental Sciences (US), University of Oslo (NO), University of Colorado Boulder (US), Chinese Academy of Sciences (CN), Czech Academy of Sciences, Astronomical Institute (CZ), Korea Astronomy and Space Science Institute (KR), Japan Aerospace Exploration Agency (JP), Institut d'Astrophysique Spatiale (FR), National Space Science Center (CN), Instituto de Astrofísica de Canarias (ES), Institute of Space and Astronautical Science (JP), Istituto Ricerche Solari Locarno (CH), NOAA National Centers for Environmental Information (US), National Astronomical Observatory of Japan (JP), Università della Svizzera italiana (CH)
National Science Foundation, National Aeronautics and Space Administration, Ministerio de Ciencia, Innovación y Universidades, European Commission, Schweizerischer Nationalfonds zur Förderung der Wissenschaftlichen Forschung, National Science Council, Centre National d’Etudes Spatiales, Akademie Věd České Republiky, Universitetet i Oslo, National Astronomical Observatory of Japan, Ames Research Center, Marshall Space Flight Center, Science and Technology Facilities Council, Japan Society for the Promotion of Science, Japan Aerospace Exploration Agency, European Regional Development Fund, Agencia Estatal de Investigación, Advanced Scientific Computing Research
Openalex Percentile: Top 7%
Solar and Space Plasma Dynamics
3.46
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