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Intensity contrast of solar network and faculae close to the solar limb, observed from two vantage points

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Intensity contrast of solar network and faculae close to the solar limb, observed from two vantage points

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dc.contributor.author	Albert, K.
dc.contributor.author	Blanco Rodríguez, Julian
dc.contributor.author	Gasent-Blesa, José Luis
dc.contributor.author	Sanchis Kilders, Esteban
dc.contributor.author	Moreno Vacas, A
dc.contributor.author	Orozco Suárez, D.
dc.contributor.author	Albelo Jorge, N.
dc.contributor.author	Alvarez Herrero, A.
dc.contributor.author	Gutiérrez Márquez, P.
dc.contributor.author	del Toro Iniesta, J. C.
dc.contributor.author	Pérez Grande, Isabel
dc.contributor.author	Balaguer Jiménez, M.
dc.contributor.author	Bellot Rubio, L.R.
dc.date.accessioned	2023-11-27T11:41:06Z
dc.date.available	2023-11-27T11:41:06Z
dc.date.issued	2023
dc.identifier.uri	https://hdl.handle.net/10550/91453
dc.description.abstract	Context. The brightness of faculae and network depends on the angle at which they are observed and the magnetic flux density. Close to the limb, the assessment of this relationship has until now been hindered by the increasingly lower signal in magnetograms. Aims. This preliminary study aims to highlight the potential of using simultaneous observations from different vantage points to better determine the properties of faculae close to the limb. Methods. We used data from the Solar Orbiter/Polarimetric and Helioseismic Imager (SO/PHI), and the Solar Dynamics Observatory/Helioseismic and Magnetic Imager (SDO/HMI), recorded at an ∼60° angular separation of their lines of sight at the Sun. We used the continuum intensity observed close to the limb by SO/PHI and complemented it with the co-observed BLOS from SDO/HMI, originating closer to disc centre (as seen by SDO/HMI), thus avoiding the degradation of the magnetic field signal near the limb. Results. We derived the dependence of facular brightness in the continuum on disc position and magnetic flux density from the combined observations of SO/PHI and SDO/HMI. Compared with a single point of view, we were able to obtain contrast values reaching closer to the limb and to lower field strengths. We find the general dependence of the limb distance at which the contrast is maximum on the flux density to be at large in line with single viewpoint observations, in that the higher the flux density is, the closer the turning point lies to the limb. There is a tendency, however, for the maximum to be reached closer to the limb when determined from two vantage points. We note that due to the preliminary nature of this study, these results must be taken with caution. Conclusions. Our analysis shows that studies involving two viewpoints can significantly improve the detection of faculae near the solar limb and the determination of their brightness contrast relative to the quiet Sun.
dc.language.iso	eng
dc.relation.ispartof	Astronomy and Astrophysics, 2023, vol. 678, num. A163, p. 1-11
dc.source	Albert, K. et al. (2023). Intensity contrast of solar network and faculae close to the solar limb, observed from two vantage points. Astronomy and Astrophysics, 678, A163. https://doi.org/10.1051/0004-6361/202346037
dc.subject	astronomia
dc.subject	astrofísica
dc.subject	física
dc.subject	electrònica
dc.subject	photosphere
dc.subject	magnetic fields
dc.subject	plages
dc.title	Intensity contrast of solar network and faculae close to the solar limb, observed from two vantage points
dc.type	journal article
dc.date.updated	2023-11-27T11:41:06Z
dc.identifier.doi	10.1051/0004-6361/202346037
dc.identifier.idgrec	162136
dc.rights.accessRights	open access