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Chromospheric observations and magnetic configuration of a supergranular structure
Stockholm University, Faculty of Science, Department of Astronomy.ORCID iD: 0000-0002-0950-9335
Stockholm University, Faculty of Science, Department of Astronomy.ORCID iD: 0000-0002-6807-1273
Stockholm University, Faculty of Science, Department of Astronomy.
Stockholm University, Faculty of Science, Department of Astronomy.ORCID iD: 0000-0002-4640-5658
Number of Authors: 42018 (English)In: Astronomy and Astrophysics, ISSN 0004-6361, E-ISSN 1432-0746, Vol. 621, article id A1Article in journal (Refereed) Published
Abstract [en]

Context. Unipolar magnetic regions are often associated with supergranular cells. The chromosphere above these regions is regulated by the magnetic field, but the field structure is poorly known. In unipolar regions, the fibrillar arrangement does not always coincide with magnetic field lines, and polarimetric observations are needed to establish the chromospheric magnetic topology. Aims. In an active region close to the limb, we observed a unipolar annular network of supergranular size. This supergranular structure harbours a radial distribution of the fibrils converging towards its centre. We aim to improve the description of this structure by determining the magnetic field configuration and the line-of-sight velocity distribution in both the photosphere and the chromosphere. Methods. We observed the supergranular structure at different heights by taking data in the Fe I 6301-6302 angstrom, H alpha, Ca II 8542 angstrom, and the Ca II H&K spectral lines with the CRisp Imaging SpectroPolarimeter (CRISP) and CHROMospheric Imaging Spectrometer (CHROMIS) at the Swedish 1-m Solar Telescope. We performed Milne-Eddington inversions of the spectropolarimetric data of Fe I 6301-6302 angstrom and applied the weak field approximation to Ca II 8542 angstrom data to retrieve the magnetic field in the photosphere and chromosphere. We used photospheric magnetograms of CRISP, Hinode Solar Optical Telescope spectropolarimeter, and Helioseismic and Magnetic Imager to calculate the magnetic flux. We investigated the velocity distribution using the line-of-sight velocities computed from the Milne-Eddington inversion and from the Doppler shift of the K-3 feature in the Ca II K spectral line. To describe the typical spectral profiles characterising the chromosphere above the inner region of the supergranular structure, we performed a K-mean clustering of the spectra in Ca II K. Results. The photospheric magnetic flux shows that the supergranular boundary has an excess of positive polarity and the whole structure is not balanced. The magnetic field vector at chromospheric heights, retrieved by the weak field approximation, indicates that the field lines within the supergranular cell tend to point inwards, and might form a canopy above the unipolar region. In the centre of the supergranular cell hosting the unipolar region, we observe a persistent chromospheric brightening coinciding with a strong gradient in the line-of-sight velocity.

Place, publisher, year, edition, pages
2018. Vol. 621, article id A1
Keywords [en]
methods: observational, Sun: chromosphere, Sun: photosphere, Sun: magnetic fields
National Category
Astronomy, Astrophysics and Cosmology
Identifiers
URN: urn:nbn:se:su:diva-165807DOI: 10.1051/0004-6361/201833246ISI: 000454396800001OAI: oai:DiVA.org:su-165807DiVA, id: diva2:1287543
Available from: 2019-02-11 Created: 2019-02-11 Last updated: 2019-12-04Bibliographically approved

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Robustini, CarolinaEsteban Pozuelo, SaraLeenaarts, Jorritde la Cruz Rodríguez, Jaime
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