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Please use this identifier to cite or link to this item: https://olympias.lib.uoi.gr/jspui/handle/123456789/40200
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dc.contributor.authorBiswal, Shreeyeshen
dc.date.accessioned2026-06-29T11:57:19Z-
dc.date.available2026-06-29T11:57:19Z-
dc.identifier.urihttps://olympias.lib.uoi.gr/jspui/handle/123456789/40200-
dc.identifier.urihttp://dx.doi.org/10.26268/heal.uoi.19843-
dc.rightsCC0 1.0 Universal*
dc.rights.urihttp://creativecommons.org/publicdomain/zero/1.0/*
dc.subjectSolar Physicsen
dc.subjectSpace Weatheren
dc.subjectSolar Flaresen
dc.subjectForecastingen
dc.subjectSolar Magnetic Fieldsen
dc.titleThree-Dimensional Solar Flare Forecastingen
dc.typedoctoralThesisen
heal.typedoctoralThesisel
heal.type.enDoctoral thesisen
heal.type.elΔιδακτορική διατριβήel
heal.classificationSolar Physicsen
heal.contributorNameBiswal, Shreeyeshen
heal.dateAvailable2026-06-29T11:58:20Z-
heal.languageenel
heal.accessfreeel
heal.recordProviderΠανεπιστήμιο Ιωαννίνων. Σχολή Θετικών Επιστημώνel
heal.publicationDate2026-06-24-
heal.abstractSolar flares are intense bursts of electromagnetic radiation spanning across the electromagnetic spectrum and are key drivers of space weather phenomena. They are closely linked to other solar energetic phenomena such as coronal mass ejections and energetic particle events which have the potential to cause damage to both satellite-based or ground-based critical electronic infrastructure. Hence prediction or forecasting of such events is of key value to space weather research. Traditional techniques related to solar flare forecasting have focused on studying these parameters on the photosphere, where the magnetic field measurements are routinely available. However, recent studies on magnetic helicity and proxy parameters of the horizontal gradient of the vertical magnetic field, have shown that extrapolating the vertical magnetic field data obtained at the photosphere to higher altitudes could potentially improve flare prediction time. In this connection, we decide to extend such an approach to (i) polarity inversion lines - lines that demarcate regions of oppositely directed vertical field regions on the solar surface and (ii) R-value, a filtered version of magnetic flux, computed in close vicinity of polarity inversion lines. In this thesis, these features are studied based on their magnitudes and temporal evolution, spanning across multiple heights in the low solar atmosphere (up to ∼ 3 Mm).en
heal.advisorNameNindos, Alexanderen
heal.committeeMemberNameGeorgoulis, Manolisen
heal.committeeMemberNameFay-Siebenburgen, Robertus vonen
heal.committeeMemberNameΝίντος, Αλέξανδροςel
heal.committeeMemberNameNindos, Alexanderen
heal.committeeMemberNameΠατσουράκος, Σπυρίδωνel
heal.committeeMemberNamePatsourakos, Spyridonen
heal.committeeMemberNameΑρχοντής, Βασίλειοςel
heal.committeeMemberNameArchontis, Vassiliosen
heal.committeeMemberNameΓοντικάκης, Κωνσταντίνοςel
heal.committeeMemberNameGontikakis, Constantinosen
heal.committeeMemberNameΜπάκας, Νικόλαοςel
heal.committeeMemberNameBakas, Nikolaosen
heal.academicPublisherΠανεπιστήμιο Ιωαννίνων. Σχολή Θετικών Επιστημών. Τμήμα Φυσικήςel
heal.academicPublisherIDuoiel
heal.numberOfPages273el
heal.fullTextAvailabilitytrue-
heal.fullTextAvailabilitytrue-
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