Journal Article

Observational Evidence of S-web Source of the Slow Solar Wind

Peter, H, Berghmans, D, Yardley, S. L, Stangalini, M, To, A. S. H, James, A. W, Smith, P, French, R. J, Cuadrado, R. Aznar, Rodriguez, L, Brooks, D. H, Perrone, D, Schuehle, U, Janvier, M, Démoulin, P, Verbeeck, C, Mihailescu, T, Owen, C. J, Baker, D, D’Amicis, R, Long, D. M, van Driel-Gesztelyi, L, Horbury, T. S, Matthews, S, Barczynski, K, Zhukov, A. N, Harra, L, Valori, G

2023

Overview

From 2022 March 18 to 21, NOAA Active Region (AR) 12967 was tracked simultaneously by Solar Orbiter at 0.35 au and Hinode/EIS at Earth. During this period, strong blueshifted plasma upflows were observed along a thin, dark corridor of open magnetic field originating at the AR’s leading polarity and continuing toward the southern extension of the northern polar coronal hole. A potential field source surface model shows large lateral expansion of the open magnetic field along the corridor. Squashing factor Q-maps of the large-scale topology further confirm super-radial expansion in support of the S-web theory for the slow wind. The thin corridor of upflows is identified as the source region of a slow solar wind stream characterized by ∼300 km s−1 velocities, low proton temperatures of ∼5 eV, extremely high density >100 cm−3, and a short interval of moderate Alfvénicity accompanied by switchback events. When the connectivity changes from the corridor to the eastern side of the AR, the in situ plasma parameters of the slow solar wind indicate a distinctly different source region. These observations provide strong evidence that the narrow open-field corridors, forming part of the S-web, produce some extreme properties in their associated solar wind streams.

• Publisher: IOP Publishing
• Subject: Coronal holes / Magnetic fields / Potential fields / Solar Orbiter (ESA) / Solar orbits / Solar wind / Topology / Webs (structural)