J/A+A/692/A191ivo://CDS.VizieR/J/A+A/692/A191doi:10.26093/cds/vizier/bc-nm/lbjbCDSGu C.Heidrich-Meisner V.Wimmer-Schweingruber R.F.2026-07-03T06:36:18Z2025-05-30T14:32:30ZCDS support team

CDS, Observatoire de Strasbourg, 11 rue de l'Universite, F-67000 Strasbourg, France

cds-question@unistra.frthe-sunObservations of the Fe and O charge states in the solar wind and interplanetary coronal mass ejections (ICMEs) generally exhibit a positive correlation between the average charge states of Fe and O (avQFe and avQO). Because Fe and O charge states freeze at different heights in the corona, this positive correlation indicates that conditions at different heights in the corona vary as a whole. We identify short time periods in the solar wind that exhibit anticorrelations between the average Fe and O charge states and investigate their properties. We aim to distinguish whether these anticorrelations are due to the related solar sources or to transport effects (e.g., differential streaming). We study kinetic properties of the solar wind related to these anticorrelated structures as well as heavy ion differential streaming in order to infer a possible relationship between conditions in coronal source regions and the reported in situ measurements. We employed a recently developed sliding-window cross-correlation method to locate anticorrelated structures in the solar wind composition measurements between 2001 and 2010 from the Advanced Composition Explorer (ACE). To account for fluctuations and measurement uncertainties, we varied the timescales and temporal lags. We determined the onset and end times of the gradual increases or decreases in the average charge states of O and Fe and analyzed the kinetic and plasma properties of the anticorrelated structures. We identified 103 anticorrelated structures both in the solar wind and in ICMEs. The behavior of avQFe is strongly related to solar wind kinetic properties, including proton speed, proton temperature, and the proton-proton collisional age. We find that the anticorrelation of avQFe and avQO during these time periods cannot be explained by differential streaming nor by unrecorded hot plasma ejections. Thus, the measured anticorrelated variations in avQFe and avQO probably indicate that changes in coronal conditions at different freeze-in heights may follow opposite monotonic trends.2024A&A...692A.191Ghttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/692/A191CatalogResearchIsServedByTAP VizieR generic servicehttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/692/A191https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/692/A191http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/692/A191https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/692/A191https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/692/A191http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/692/A191GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapdefaultJ/A+A/692/A191/appendixList of the 103 anti-correlated structures identified in paperrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintSeq[1/103] Event sequence numbermeta.id;meta.mainintYearYearyrtimeintST1The start time of Fe signal, in day of year, based on the weak solutiondstat.snr;time.startdoubleET1The end time of Fe signal, in day of year, based on the weak solutiondstat.snr;time.enddoubleST2The start time of O signal, in day of year, based on the weak solutiondstat.snr;time.startdoubleET2The end time of O signal, in day of year, based on the weak solutiondstat.snr;time.enddoubleST3The start time of Fe signal, in day of year, based on the strong solutiondstat.snr;time.startdoubleET3The end time time of Fe signal, in day of year, based on the strong solutiondstat.snr;time.enddoubleST4The start time of O signal, in day of year, based on the strong solutiondstat.snr;time.startdoubleET4The end time time of O signal, in day of year, based on the strong solutiondstat.snr;time.enddouble