Magnetic topology, coronal outflows, and the solar wind

MANDRINI, C.H.; VAN DRIEL-GESZTELYI, L.; DÉMOULIN, P.; CULHANE, J.L.; BAKER, D.; DEROSA, M.L.; ROUILLARD, A.P.; OPITZ, A.; STENBORG, G.; VOURLIDAS, A.; BROOKS, D.H.

Mysore

Congreso; 39th COSPAR General Assembly; 2012

COSPAR

During 2-18 January 2008 a pair of low-latitude opposite polarity coronal holes were observed on the Sun anked by two ARs with the heliospheric plasma sheet between them. Hinode/EUV Imaging Telescope (EIS) is used to locate AR-related outows and measure their velocities. The Advanced Composition Explorer (ACE) in-situ observations are employed to assess the resulting impacts on the interplanetary solar wind (SW). Magnetic eld extrapolations of the two ARs conrm that AR plasma outows observed with EIS are co-spatial with quasi-separatrix layer locations, including the separatrix of a null point. Global potential eld source-surface modeling indicates that eld lines in the vicinity of the null point extend up to the source-surface, enabling a part of the EIS plasma upows access to the SW. Similar upow magnitude is also observed within closed eld regions. Though part of the plasma upows observed with EIS remain conned along closed coronal loops, a subset of them are indeed able to make their imprint in the slow SW, making ARs bordering coronal holes a slow SW contributor.