{"id":{"repo_id":"qu-belfast","oai_identifier":"oai:pure.qub.ac.uk/portal:studenttheses/345b051b-f2de-49ef-8af0-3cea65476576"},"canonical_url":"https://search.dev.ndltd.org/etd/qu-belfast/oai:pure.qub.ac.uk/portal:studenttheses/345b051b-f2de-49ef-8af0-3cea65476576","repository":{"repo_id":"qu-belfast","name":"Queen's University Belfast","base_url":"https://pureadmin.qub.ac.uk/ws/oai"},"display":{"title":"Analysis and Modelling of a Type II White-light Solar Flare","abstract":"Type II white-light flares (WLFs) are rare impulsive events in solar atmosphere observed across the electromagnetic spectrum, but without the characteristic emission in hydrogen lines. A unique set of multi-instrument observations is presented with broad wavelength range spectra in the visible and UV range. Data from the RHESSI and Fermi satellites provide evidence of both non-thermal electron and proton beams during the studied flare. The observations put important constraints on the beam parameters and allow a deeper investigation using radiative hydrodynamic modelling.<br/> <br/> Radiative hydrodynamic simulations show that the observed flare signatures cannot be<br/>explained with ‘standard’ electron beams, since such beams deposit at least part of their energy in the upper chromosphere where hydrogen lines are formed. Instead, the models suggest that the beams penetrate through the upper chromosphere and deliver their energy directly into the lower chromosphere. Such beams can be dominated by both electrons and/or protons, but electron beams require rather exotic parameters. On the other hand, proton beams penetrate easily through the upper chromosphere and deliver enough energy to power the white-light emission while their energy flux can remain<br/>relatively low.<br/><br/> The models show that the previously reported time lag between the X-ray emission and WL emission is not a type II WLFs’ feature, instead these events do not show radiative losses via Lyman emission originating in the top chromosphere. The WL continuum is dominated by free-bound hydrogen emission originating in the mid-lower chromosphere.<br/>","abstract_html":"Type II white-light flares (WLFs) are rare impulsive events in solar atmosphere observed across the electromagnetic spectrum, but without the characteristic emission in hydrogen lines. A unique set of multi-instrument observations is presented with broad wavelength range spectra in the visible and UV range. Data from the RHESSI and Fermi satellites provide evidence of both non-thermal electron and proton beams during the studied flare. The observations put important constraints on the beam parameters and allow a deeper investigation using radiative hydrodynamic modelling.&lt;br/&gt; &lt;br/&gt; Radiative hydrodynamic simulations show that the observed flare signatures cannot be&lt;br/&gt;explained with ‘standard’ electron beams, since such beams deposit at least part of their energy in the upper chromosphere where hydrogen lines are formed. Instead, the models suggest that the beams penetrate through the upper chromosphere and deliver their energy directly into the lower chromosphere. Such beams can be dominated by both electrons and/or protons, but electron beams require rather exotic parameters. On the other hand, proton beams penetrate easily through the upper chromosphere and deliver enough energy to power the white-light emission while their energy flux can remain&lt;br/&gt;relatively low.&lt;br/&gt;&lt;br/&gt; The models show that the previously reported time lag between the X-ray emission and WL emission is not a type II WLFs’ feature, instead these events do not show radiative losses via Lyman emission originating in the top chromosphere. The WL continuum is dominated by free-bound hydrogen emission originating in the mid-lower chromosphere.&lt;br/&gt;","abstract_has_math":false,"creators":["Procházka, Ondrej"],"institution":"Queen's University Belfast","degree_name":"Doctor of Philosophy","degree_level":"Doctoral Thesis","degree_discipline":null,"degree_department":null,"school":null,"contributors":[],"advisors":["Mathioudakis, Mihalis"],"committee_chairs":[],"committee_members":[],"year":2019,"date_issued":"2019","date_published":"2019","updated_at":"2026-07-24T03:54:59Z","subjects":[],"languages":["eng"],"rights":[],"rights_urls":[],"identifier_entries":[{"key":"dc:identifier","label":"Identifier","values":["oai:pure.qub.ac.uk/portal:studenttheses/345b051b-f2de-49ef-8af0-3cea65476576"],"render_values":[{"text":"oai:pure.qub.ac.uk/portal:studenttheses/345b051b-f2de-49ef-8af0-3cea65476576","href":null,"code":true}]}]},"links":{"outbound_url":"https://pure.qub.ac.uk/en/studentTheses/345b051b-f2de-49ef-8af0-3cea65476576","outbound_label":"Repository record","outbound_source":"dc:identifier"},"metadata_groups":[{"id":"people","label":"People","entries":[{"key":"dc:contributor.advisor","label":"Advisor","values":["Mathioudakis, Mihalis"]},{"key":"dc:creator","label":"Author","values":["Procházka, Ondrej"]}]},{"id":"academic_context","label":"Academic Context","entries":[{"key":"dc:date","label":"Dc Date","values":["2019"]},{"key":"dc:date.issued","label":"Date","values":["2019"]},{"key":"dc:publisher.department","label":"Dc Publisher Department","values":["School of Mathematics and Physics"]},{"key":"dc:publisher.institution","label":"Dc Publisher Institution","values":["Queen's University Belfast"]},{"key":"dc:relation.isreferencedby","label":"Dc Relation Isreferencedby","values":["https://pure.qub.ac.uk/en/studentTheses/345b051b-f2de-49ef-8af0-3cea65476576"]},{"key":"dc:type","label":"Dc Type","values":["Thesis"]},{"key":"dc:type.qualificationlevel","label":"Dc Type Qualificationlevel","values":["Doctoral Thesis"]},{"key":"dc:type.qualificationname","label":"Dc Type Qualificationname","values":["Doctor of Philosophy"]}]},{"id":"language_rights","label":"Language and Rights","entries":[{"key":"dc:language","label":"Dc Language","values":["eng"]}]},{"id":"identifiers","label":"Identifiers","entries":[{"key":"dc:identifier","label":"Identifier","values":["oai:pure.qub.ac.uk/portal:studenttheses/345b051b-f2de-49ef-8af0-3cea65476576","https://pure.qub.ac.uk/en/studentTheses/345b051b-f2de-49ef-8af0-3cea65476576"]},{"key":"dc:identifier.uri","label":"Identifier URI","values":["https://pure.qub.ac.uk/files/166816775/thesis_hmc.pdf"]}]},{"id":"additional","label":"Additional Metadata","entries":[{"key":"dc:description.abstract","label":"Abstract","values":["Type II white-light flares (WLFs) are rare impulsive events in solar atmosphere observed across the electromagnetic spectrum, but without the characteristic emission in hydrogen lines. A unique set of multi-instrument observations is presented with broad wavelength range spectra in the visible and UV range. Data from the RHESSI and Fermi satellites provide evidence of both non-thermal electron and proton beams during the studied flare. The observations put important constraints on the beam parameters and allow a deeper investigation using radiative hydrodynamic modelling.<br/> <br/> Radiative hydrodynamic simulations show that the observed flare signatures cannot be<br/>explained with ‘standard’ electron beams, since such beams deposit at least part of their energy in the upper chromosphere where hydrogen lines are formed. Instead, the models suggest that the beams penetrate through the upper chromosphere and deliver their energy directly into the lower chromosphere. Such beams can be dominated by both electrons and/or protons, but electron beams require rather exotic parameters. On the other hand, proton beams penetrate easily through the upper chromosphere and deliver enough energy to power the white-light emission while their energy flux can remain<br/>relatively low.<br/><br/> The models show that the previously reported time lag between the X-ray emission and WL emission is not a type II WLFs’ feature, instead these events do not show radiative losses via Lyman emission originating in the top chromosphere. The WL continuum is dominated by free-bound hydrogen emission originating in the mid-lower chromosphere.<br/>"]},{"key":"dc:title","label":"Title","values":["Analysis and Modelling of a Type II White-light Solar Flare"]}]}],"canonical_facts":{"dc:contributor.advisor":["Mathioudakis, Mihalis"],"dc:creator":["Procházka, Ondrej"],"dc:date":["2019"],"dc:date.issued":["2019"],"dc:description.abstract":["Type II white-light flares (WLFs) are rare impulsive events in solar atmosphere observed across the electromagnetic spectrum, but without the characteristic emission in hydrogen lines. A unique set of multi-instrument observations is presented with broad wavelength range spectra in the visible and UV range. Data from the RHESSI and Fermi satellites provide evidence of both non-thermal electron and proton beams during the studied flare. The observations put important constraints on the beam parameters and allow a deeper investigation using radiative hydrodynamic modelling.<br/> <br/> Radiative hydrodynamic simulations show that the observed flare signatures cannot be<br/>explained with ‘standard’ electron beams, since such beams deposit at least part of their energy in the upper chromosphere where hydrogen lines are formed. Instead, the models suggest that the beams penetrate through the upper chromosphere and deliver their energy directly into the lower chromosphere. Such beams can be dominated by both electrons and/or protons, but electron beams require rather exotic parameters. On the other hand, proton beams penetrate easily through the upper chromosphere and deliver enough energy to power the white-light emission while their energy flux can remain<br/>relatively low.<br/><br/> The models show that the previously reported time lag between the X-ray emission and WL emission is not a type II WLFs’ feature, instead these events do not show radiative losses via Lyman emission originating in the top chromosphere. The WL continuum is dominated by free-bound hydrogen emission originating in the mid-lower chromosphere.<br/>"],"dc:identifier":["oai:pure.qub.ac.uk/portal:studenttheses/345b051b-f2de-49ef-8af0-3cea65476576","https://pure.qub.ac.uk/en/studentTheses/345b051b-f2de-49ef-8af0-3cea65476576"],"dc:identifier.uri":["https://pure.qub.ac.uk/files/166816775/thesis_hmc.pdf"],"dc:language":["eng"],"dc:publisher.department":["School of Mathematics and Physics"],"dc:publisher.institution":["Queen's University Belfast"],"dc:relation.isreferencedby":["https://pure.qub.ac.uk/en/studentTheses/345b051b-f2de-49ef-8af0-3cea65476576"],"dc:title":["Analysis and Modelling of a Type II White-light Solar Flare"],"dc:type":["Thesis"],"dc:type.qualificationlevel":["Doctoral Thesis"],"dc:type.qualificationname":["Doctor of Philosophy"]},"updated_at":"2026-07-24T03:54:59Z"}