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Chromospheric observations and magnetic configuration of a supergranular structure
Stockholms universitet, Naturvetenskapliga fakulteten, Institutionen för astronomi.ORCID-id: 0000-0002-0950-9335
Stockholms universitet, Naturvetenskapliga fakulteten, Institutionen för astronomi.ORCID-id: 0000-0002-6807-1273
Stockholms universitet, Naturvetenskapliga fakulteten, Institutionen för astronomi.
Stockholms universitet, Naturvetenskapliga fakulteten, Institutionen för astronomi.ORCID-id: 0000-0002-4640-5658
Rekke forfattare: 42018 (engelsk)Inngår i: Astronomy and Astrophysics, ISSN 0004-6361, E-ISSN 1432-0746, Vol. 621, artikkel-id A1Artikkel i tidsskrift (Fagfellevurdert) 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.

sted, utgiver, år, opplag, sider
2018. Vol. 621, artikkel-id A1
Emneord [en]
methods: observational, Sun: chromosphere, Sun: photosphere, Sun: magnetic fields
HSV kategori
Identifikatorer
URN: urn:nbn:se:su:diva-165807DOI: 10.1051/0004-6361/201833246ISI: 000454396800001OAI: oai:DiVA.org:su-165807DiVA, id: diva2:1287543
Tilgjengelig fra: 2019-02-11 Laget: 2019-02-11 Sist oppdatert: 2019-12-04bibliografisk kontrollert

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