Identifying the Coronal Source Regions of Solar Wind Streams from Total Solar Eclipse Observations and in situ Measurements Extending over a Solar Cycle

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dc.contributor.authorHabbal, Shadia Rifaics
dc.contributor.authorDruckmüller, Miloslavcs
dc.contributor.authorNathalia, Alzatecs
dc.contributor.authorDing, Adalbertcs
dc.contributor.authorJohnson, Juddcs
dc.contributor.authorŠtarha, Pavelcs
dc.contributor.authorHoderová, Janacs
dc.contributor.authorBoe, Benjamincs
dc.contributor.authorConstantiniou, Sagecs
dc.contributor.authorArndt, Martinacs
dc.coverage.issue1cs
dc.coverage.volume911cs
dc.date.accessioned2021-08-13T10:52:54Z
dc.date.available2021-08-13T10:52:54Z
dc.date.issued2021-04-12cs
dc.description.abstractThis letter capitalizes on a unique set of total solar eclipse observations acquired between 2006 and 2020 in white light, Fe xi 789.2 nm (T-fexi = 1.2 0.1 MK), and Fe xiv 530.3 nm (T-fexiv = 1.8 0.1 MK) emission complemented by in situ Fe charge state and proton speed measurements from Advanced Composition Explorer/SWEPAM-SWICS to identify the source regions of different solar wind streams. The eclipse observations reveal the ubiquity of open structures invariably associated with Fe xi emission from Fe10+ and hence a constant electron temperature, T-c = T-fexi, in the expanding corona. The in situ Fe charge states are found to cluster around Fe10+, independently of the 300-700 km s(-1) stream speeds, referred to as the continual solar wind. Thus, Fe10+ yields the fiducial link between the continual solar wind and its T-fexi sources at the Sun. While the spatial distribution of Fe xiv emission from Fe13+ associated with streamers changes throughout the solar cycle, the sporadic appearance of charge states >Fe11+ in situ exhibits no cycle dependence regardless of speed. These latter streams are conjectured to be released from hot coronal plasmas at temperatures >= T-fexiv within the bulge of streamers and from active regions, driven by the dynamic behavior of prominences magnetically linked to them. The discovery of continual streams of slow, intermediate, and fast solar wind characterized by the same T-fexi in the expanding corona places new constraints on the physical processes shaping the solar wind.en
dc.formattextcs
dc.format.extent1-14cs
dc.format.mimetypeapplication/pdfcs
dc.identifier.citationAstrophysical Journal Letters. 2021, vol. 911, issue 1, p. 1-14.en
dc.identifier.doi10.3847/2041-8213/abe775cs
dc.identifier.issn2041-8205cs
dc.identifier.other171593cs
dc.identifier.urihttp://hdl.handle.net/11012/200986
dc.language.isoencs
dc.publisherIOP PUBLISHING LTDcs
dc.relation.ispartofAstrophysical Journal Letterscs
dc.relation.urihttps://iopscience.iop.org/article/10.3847/2041-8213/abe775/pdfcs
dc.rightsCreative Commons Attribution 4.0 Internationalcs
dc.rights.accessopenAccesscs
dc.rights.sherpahttp://www.sherpa.ac.uk/romeo/issn/2041-8205/cs
dc.rights.urihttp://creativecommons.org/licenses/by/4.0/cs
dc.subjectSolar prominencesen
dc.subjectSolar cycleen
dc.subjectSolar winden
dc.subjectTotal eclipsesen
dc.subjectSolar coronal streamersen
dc.subjectSolar magnetic fieldsen
dc.subjectSolar coronal heatingen
dc.subjectSolar coronal mass ejectionsen
dc.subjectSolar coronaen
dc.titleIdentifying the Coronal Source Regions of Solar Wind Streams from Total Solar Eclipse Observations and in situ Measurements Extending over a Solar Cycleen
dc.type.driverarticleen
dc.type.statusPeer-revieweden
dc.type.versionpublishedVersionen
sync.item.dbidVAV-171593en
sync.item.dbtypeVAVen
sync.item.insts2021.08.13 12:52:54en
sync.item.modts2021.08.13 12:14:08en
thesis.grantorVysoké učení technické v Brně. Fakulta strojního inženýrství. Ústav matematikycs
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