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Coronal voids and their magnetic nature

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Coronal voids and their magnetic nature

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dc.contributor.author	Nölke, J.D.
dc.contributor.author	Blanco Rodríguez, Julian
dc.contributor.author	Gasent-Blesa, José Luis
dc.contributor.author	Sanchis Kilders, Esteban
dc.contributor.author	Gutiérrez Márquez, P.
dc.contributor.author	Orozco Suárez, D.
dc.contributor.author	Albelo Jorge, N.
dc.contributor.author	Alvarez Herrero, A.
dc.contributor.author	Pérez Grande, Isabel
dc.contributor.author	del Toro Iniesta, J.C.
dc.contributor.author	Balaguer Jiménez, M.
dc.date.accessioned	2023-11-27T11:13:00Z
dc.date.available	2023-11-27T11:13:00Z
dc.date.issued	2023
dc.identifier.uri	https://hdl.handle.net/10550/91451
dc.description.abstract	Context. Extreme ultraviolet (EUV) observations of the quiet solar atmosphere reveal extended regions of weak emission compared to the ambient quiescent corona. The magnetic nature of these coronal features is not well understood. Aims. We study the magnetic properties of the weakly emitting extended regions, which we name coronal voids. In particular, we aim to understand whether these voids result from a reduced heat input into the corona or if they are associated with mainly unipolar and possibly open magnetic fields, similar to coronal holes. Methods. We defined the coronal voids via an intensity threshold of 75% of the mean quiet-Sun (QS) EUV intensity observed by the high-resolution EUV channel (HRIEUV) of the Extreme Ultraviolet Imager on Solar Orbiter. The line-of-sight magnetograms of the same solar region recorded by the High Resolution Telescope of the Polarimetric and Helioseismic Imager allowed us to compare the photospheric magnetic field beneath the coronal voids with that in other parts of the QS. Results. The coronal voids studied here range in size from a few granules to a few supergranules and on average exhibit a reduced intensity of 67% of the mean value of the entire field of view. The magnetic flux density in the photosphere below the voids is 76% (or more) lower than in the surrounding QS. Specifically, the coronal voids show much weaker or no network structures. The detected flux imbalances fall in the range of imbalances found in QS areas of the same size. Conclusions. We conclude that coronal voids form because of locally reduced heating of the corona due to reduced magnetic flux density in the photosphere. This makes them a distinct class of (dark) structure, different from coronal holes.
dc.language.iso	eng
dc.relation.ispartof	Astronomy and Astrophysics, 2023, vol. 678, num. A196, p. 1-10
dc.source	Nölke, J.D. et al. (2023). Coronal voids and their magnetic nature. Astronomy and Astrophysics, 678, A196. https://doi.org/10.1051/0004-6361/202346040
dc.subject	astronomia
dc.subject	astrofísica
dc.subject	física
dc.subject	electrònica
dc.subject	photosphere
dc.subject	magnetic fields
dc.subject	atmosphere
dc.title	Coronal voids and their magnetic nature
dc.type	journal article
dc.date.updated	2023-11-27T11:13:01Z
dc.identifier.doi	10.1051/0004-6361/202346040
dc.identifier.idgrec	162134
dc.rights.accessRights	open access