Μελέτη ανάδυσης μαγνητικής ροής στην ηλιακή ατμόσφαιρα με χρήση αριθμητικών προσομοιώσεων
| dc.contributor.author | Καραντάνης, Ευάγγελος | el |
| dc.contributor.author | Karantanis, Evangelos | en |
| dc.date.accessioned | 2025-01-27T12:01:56Z | |
| dc.date.available | 2025-01-27T12:01:56Z | |
| dc.identifier.uri | https://olympias.lib.uoi.gr/jspui/handle/123456789/38709 | |
| dc.rights | Default License | |
| dc.subject | Ήλιος | el |
| dc.subject | Μαγνητοϋδροδυναμική | el |
| dc.subject | Ανάδυση μαγνητικής ροής | el |
| dc.subject | Sun | en |
| dc.subject | Magnetohydrodynamics | en |
| dc.subject | Magnetic flux emergence | en |
| dc.title | Μελέτη ανάδυσης μαγνητικής ροής στην ηλιακή ατμόσφαιρα με χρήση αριθμητικών προσομοιώσεων | el |
| dc.title | Study of magnetic flux emergence in the solar atmosphere using numerical simulations | en |
| dc.type | masterThesis | en |
| heal.abstract | The subject of this master thesis is the study of magnetic flux emergence in the solar atmosphere using numerical simulations. It is well known that various phenomena in the Sun such as solar flares, jets, coronal mass ejections (CME), are linked to magnetic structures beneath the photosphere. These structures transport magnetic flux from the deep convection zone to the photosphere and then expand in the corona. In this thesis we focus on the interaction between the emerging magnetic field and the external ambient field leading to standard jet formation and more intense eruptions known as blowout jets. To quantify the amount of energy and magnetic field transported into the solar atmosphere we conduct three-dimensional (3D), resistive magnetohydrodynamic (MHD) numerical simulations using Lare3D code. This allows us to model the emergence process and the eruptive phenomena produced in our simulations. The magnetic flux is concentrated along rigid structures located in the convection zone and we examine different topologies of those structures to understand how their characteristics affect the amount of energy that can emerge and produce transient phenomena. Given the importance of the twist of the field lines in a flux tube, we compare cases with higher (α = 0.4) and lower (α = 0.1) twists. For the high twist case (α = 0.4) we find that both tubes produce multiple jets and blowout jets. The horizontal tube releases a significant amount of energy in the corona as compared to the toroidal tube however the toroidal tube maintains an eruptive behavior for longer time albeit with less intensity. We find that the reasons behind these behavior is that the toroidal tube maintains and increases the amount of axial flux located at the upper atmosphere whereas the horizontal tube after the first two intense eruptions can no longer create and maintain axial flux which is an important factor since it is linked to the twisted magnetic field lines that lead to eruptions. For the less twisted case (α = 0.1) the toroidal tube cannot produce any eruptions given that the field lines emergence with almost no twist and there is no further shearing motion. The horizontal tube, due to its undulation produces one eruption. Overall, the geometrical structure of real magnetic flux tubes in the Sun is not well established therefore numerical simulations can help identify these structures by comparing them with observational data from eruptive phenomena on the Sun. | en |
| heal.academicPublisher | Πανεπιστήμιο Ιωαννίνων. Σχολή Θετικών Επιστημών. Τμήμα Φυσικής | el |
| heal.academicPublisher | University of Ioannina. School of Sciences. Department of Physics | en |
| heal.academicPublisherID | uoi | el |
| heal.access | free | el |
| heal.advisorName | Αρχοντής, Βασίλης | el |
| heal.classification | Ηλιακή φυσική | el |
| heal.classification | Solar physics | en |
| heal.committeeMemberName | Αρχοντής, Βασίλης | el |
| heal.committeeMemberName | Νίντος, Αλέξανδρος | el |
| heal.committeeMemberName | Πατσουράκος, Σπύρος | el |
| heal.dateAvailable | 2025-01-27T12:02:56Z | |
| heal.fullTextAvailability | true | |
| heal.language | en | el |
| heal.numberOfPages | 83 | el |
| heal.publicationDate | 2025-01-15 | |
| heal.recordProvider | Πανεπιστήμιο Ιωαννίνων. Σχολή Θετικών Επιστημών | el |
| heal.recordProvider | University of Ioannina. School of Sciences | en |
| heal.type | masterThesis | el |
| heal.type.el | Μεταπτυχιακή εργασία | el |
| heal.type.en | Master thesis | en |
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