2015/04/30 by Hui Fu, Bo Li, Xing Li +4 · 39 citations
Biochemistry, Genetics and Molecular Biology · Physics and Astronomy · #Context (archaeology) #Coronal hole #Coronal loop #Coronal mass ejection #Flux (metallurgy) #Geomagnetism and Paleomagnetism Studies #Ionosphere and magnetosphere dynamics #Nanoflares #Solar and Space Plasma Dynamics #Solar minimum #Solar physics #Solar wind #astro-ph.SR
paper · pdf · doi:10.1007/s11207-015-0689-9
published in Solar Physics 290(5), 1399-1415 (Springer Science+Business Media) · 24 pages, 7 figures, accepted for publication in Solar Physics
openalex publication_date 2015/04/30 · arxiv created 2015/05/03 · arxiv updated 2015/05/05 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/05
We identify the coronal sources of the solar winds sampled by the ACE spacecraft during 1999-2008, and examine the in situ solar wind properties as a function of wind sources. The standard two-step mapping technique is adopted to establish the photospheric footpoints of the magnetic flux tubes along which the ACE winds flow. The footpoints are then placed in the context of EIT 284~Å images and photospheric magnetograms, allowing us to categorize the sources into four groups: coronal holes (CHs), active regions (ARs), the quiet Sun (QS), and "Undefined". This practice also enables us to establish the response to solar activity of the fractions occupied by each kind of solar winds, and of their speeds and O7+/O6+ ratios measured in situ. We find that during the maximum phase, the majority of ACE winds originate from ARs. During the declining phase, CHs and ARs are equally important contributors to the ACE solar winds. The QS contribution increases with decreasing solar activity, and maximizes in the minimum phase when QS appear to be the primary supplier of the ACE winds. With decreasing activity, the winds from all sources tend to become cooler, as represented by the increasingly low O7+/O6+ ratios. On the other hand, during each activity phase, the AR winds tend to be the slowest and associated with the highest O7+/O6+ ratios, and the CH winds correspond to the other extreme, with the QS winds lying in between. Applying the same analysis method to the slow winds only, here defined as the winds with speeds lower than 500 km s-1, we find basically the same overall behavior, as far as the contributions of individual groups of sources are concerned. This statistical study indicates that QS regions are an important source of the solar wind during the minimum phase.