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京都大学 / 新制・課程博士 / 博士(理学) / 甲第24414号 / 理博第4913号 / 新制||理||1702(附属図書館) / 京都大学大学院理学研究科物理学・宇宙物理学専攻 / (主査)准教授 浅井 歩, 教授 一本 潔, 教授 横山 央明 / 学位規則第4条第1項該当 / Doctor of Science / Kyoto University / DFAM

This work serves to present the background, approach, and selected results for the initial master thesis and prototyping phase of Open Space, a joint visualization software development project by National Aeronautics and Space Administration (NASA), Linköping University (LiU) and the American Museum of Natural History (AMNH). The thesis report provides a theoretical introduction to heliophysics, modeling of space weather events, volumetric rendering, and an understanding of how these relate in the bigger scope of Open Space. A set of visualization tools that are currently used at NASA and AMNH are presented and discussed. These tools are used to visualize global heliosphere models, both for scientific studies and for public presentations, and are mainly making use of geometric rendering techniques. The paper will, in detail, describe a new approach to visualize the science models with volumetric rendering to better represent the volumetric structure of the data. Custom processors have been developed for the open source volumetric rendering engine Voreen, to load and visualize science models provided by the Community Coordinated Modeling Center (CCMC) at NASA Goddard Space Flight Center (GSFC). Selected parts of the code are presented by C++ code examples. To best represent models that are defined in non-Cartesian space, a new approach to volumetric rendering is presented and discussed. Compared to the traditional approach of transforming such models to Cartesian space, this new approach performs no such model transformations, and thus minimizes the amount of empty voxels and introduces less interpolation artifacts. Final results are presented as rendered images and are discussed from a scientific visualization perspective, taking into account the physics representation, potential rendering artifacts, and the rendering performance.

Les ceintures de radiation correspondent à la région de la magnétosphère dans laquelle se trouvent les particules de hautes énergies. Le couplage entre le vent solaire et la magnétosphère donne lieu à des variations des flux de particules sur plusieurs ordres de grandeurs. L’objectif de cette thèse est d’observer et caractériser ces variations de flux d’électrons au passage de différents types d’événements tels que les régions d’interaction en co-rotation (CIRs) et les éjections de masse coronale interplanétaires (ICMEs). Pour cela, nous avons traité et analysé les données de plusieurs types: paramètres du vent solaire, indices géomagnétiques et flux d’électrons dans les ceintures de radiation. Dans les trois premiers chapitres, nous rendons compte de la complexité de l’environnement spatial Terrestre et présentons les différentes données utilisées. Les travaux de thèse sont ensuite organisés en quatre chapitres. Premièrement, nous utilisons les mesures des satellites NOAA-POES afin de caractériser les flux d’électrons dans les ceintures. Nous étudions ensuite les différences de variations de flux causées par les CIRs et les ICMEs en fonction de l’énergie des électrons et du paramètre L*. Après avoir montré le fort lien entre les intensités d’orages magnétiques et les variations de flux, nous nous focalisons sur les ICMEs et la variabilité des orages qu’elles causent. Enfin, nous insistons sur l’importance des enchaînements d’événements. Après avoir quantifié la forte tendance qu’ont les ICMEs à former des séquences, nous réalisons une étude statistique sur les orages qu’elles causent, puis trois études de cas afin d’illustrer leurs effets sur les ceintures. / The radiation belts are the toroidal region within the inner magnetosphere where high energetic particles are located. The coupling between the solar wind and the magnetosphere leads to strong variations of particle fluxes that can therefore increase or decrease over several orders of magnitude. The aim of this thesis is to observe and characterize the variations of fluxes during the crossing of several types of events originating from the sun such as Corotating Interaction Regions (CIRs) and Interplanetary Coronal Mass Ejections (ICMEs). To do so, we processed and analyzed the data of various types : solar wind parameters, geomagnetic indices, and electron fluxes within the radiation belts. In the three first chapters, we report on the complexity of the Terrestrial space environment and we present the Solar-Terrestrial system and the data used. Then, our work is organized around four chapters. First, we characterized the electron fluxes within the radiation belts as measured by the NOAA-POES spacecrafts. Then, we studied the difference between the variations of fluxes caused by the CIRs and the ICMEs depending on the energy and the L* parameter. After establishing strong links between the intensity of magnetic storms and the variations of fluxes, we focused on the ICMEs and the variability of the related magnetic storms. Eventually, we emphasized the importance of the sequences of events. After quantifying the trend of the ICMEs to form sequences, we performed a statistical study on the magnetic storms caused by such sequences. Finally three study cases were performed in order to illustrate the various possible effects on the radiation belts.

Coronal mass ejections (CMEs) are some of the extraterrestrialevents most impactful to earth. Eorts to model and predict theireects have seen new possibilities in the two most recent decades dueto multiple new spacecrafts providing a wider range of data than everbefore. Models of these events suer from a number of inaccuracies,one of them being the density ratio between the CME and the ambientsolar wind. Since the arrival time for potentially harmful disturbancespredicted by models has been proved to be highly sensitive to thisparameter we therefore take care to set it as accurately as possible.Traditionally this value is either set to a default, justied by denitionand theory, or set to the density ratio between the bulk if the ejectedgas and the surrounding medium. A proposition has been made tomeasure density enhancement dierently, using a reference point at theshock wave preceding the CME for each event. This method strives toimprove arrival time predictions and was in this paper tested for onecoronal mass ejection event. Two runs if the model WSA-ENLIL+Conewas made; one with the default value of density enhancement, onewith a value determined through the revised method using coronographdata. Running the model with the revised value improved the predictedarrival time by moving it forwards in time by 4h, which was still tooearly. Other input data into the model run was then discussed as apossible cause of the remaining inaccuracy. / Koronamassutkastningar är ett av solfenomenen som påverkar jorden mest.Nya rymdfarkoster med instrument som satts i arbete de senaste två decenniernahar gett data som gjort det möjligt att modellera och förutse dessaevent till en högre precision än någonsin. Alla dessa modeller lider av någonform av felkälla, en av vilka är kvoten mellan densitet för massutkastningenoch den omgivande miljön. Eftersom förutsedda ankomsstider för potentielltskadliga störningar har visat sig vara särskilt känsliga för denna parameterså tar vi särskild hänsyn till att ange den så precist som möjligt. Vanligtvissätts detta värde till ett fast standardvärde, som anges av dess denitionoch bakomliggande teori, eller till kvoten mellan utkastningens bulk ochomgivningen. Ett förslag har dock lagts fram om att omdeniera parametern.Denna metod strävar efter att förbättra förutsedda ankomsttider ochhar i denna text testats för en koronamassutkastning. Två körningar avmodellen WSA-ENLIL+Cone gjordes; en med defaultvärdet för densitetsratiot,en med värdet satt genom mätning av empirisk cononagrafdata enligtden föreslagna metoden. Att köra modellen med den nya parametern förbättrade den förutsedda ankomsttiden genom att ytta den framåt i tidenmed 4 timmar, vilket fortfarande är för tidigt. Andra inputdata i modellendiskuterades då som möjliga orsaker till den återstående diskrepansen.

Made available in DSpace on 2016-03-15T19:35:53Z (GMT). No. of bitstreams: 1 Ray Fernando Hidalgo Ramirez.pdf: 3985319 bytes, checksum: 0a36b0e596cb2c3f1eadaccfa8f843ee (MD5) Previous issue date: 2015-06-17 / Universidade Presbiteriana Mackenzie / Solar flares radio emissions provide detailed information on the energy release, particle acceleration, heating processes and plasma conditions at the sites where the radiation is generated. This study focuses in radio emission from millimeter, sub-millimeter and another complementary wavelengths obtained by recent observations that might improve the understanding of processes from the low chromosphere to the corona. Here we study a GOES class X1.7 flare on January 27, 2012 detected by the Solar Sub-millimeter Telescope (SST) at 212 and 405 GHz, and by the solar radio polarimeters (POEMAS) at 45 and 90 GHz. LASCO C2 coronagraph observed a coronal mass ejection (CME) with possible physical connection with phenomena observed at radio-frequencies, including changes in polarization degree (45 and 90 GHz) and enhancements of scintillation index (212 and 405 GHz). The complementary radio observations were obtained by the Radio Solar Telescopes Network (RSTN) at the single frequencies 0.2, 0.4, 0.6, 1.4, 2.7, 4.9, 8.8 and 15.4 GHz and at the 25 - 180 MHz band, and by the Green Bank Solar Radio Burst Spectrometer (GBSRBS) at the 100 - 300 MHz and 300 - 1200 MHz bands. The solar flare exhibits a complex time structure at microwaves consisting of three major enhancements. Type III-like metric and decametric bursts were accompanied by small polarized burst at 45 and 90 GHz with polarization degrees of 0.09 and 0.12, suggesting changes in the magnetic field strength the order of 700 and 2000 G, respectively. SST detected one impulsive burst and significant 10% enhancements of scintillation index intermittently throughout the event. The CME launch time inferred by back extrapolation of the LASCO coronagraph observations to the solar limb coincides approximately in time to the changes in polarization degree, suggesting that CME might be a result of a magnetic transient causing an instability generating the subsequent impulsive structures. / As emissões em rádio das explosões solares provém informações detalhadas dos processos de liberação de energia, aceleração de partículas, aquecimento e condições do plasma na região onde a radiação é gerada. Este estudo concentra-se em rádio emissões nos comprimentos de onda milimétricos, sub-milimétricos e outras frequências complementares obtidas por observações recentes que podem melhorar o entendimento dos processos na baixa cromosfera até a coroa. Foi estudada uma explosão solar classe GOES X1.7 ocorrida no dia 27 de janeiro de 2012, detectada pelo Telescópio Solar Sub-milimétrico (SST) em 212 e 405 GHz e pelos rádio polarímetros solares em 45 e 90 GHz. Uma ejeção de massa coronal (CME) foi observada pelo coronógrafo C2 de LASCO com possível conexão física com os fenômenos observados em rádio frequências, incluindo mudanças no grau de polarização (45 e 90 GHz) e aumentos no índice de cintilação (212 e 405 GHz). As rádio observações complementares foram obtidas em frequências distintas, pela Rede de Rádio Telescópios Solares (RSTN), de 0,2; 0,4; 0,6; 1,4; 2,7; 4,9; 8,8 e 15,4 GHz e nas faixas de 25 - 180 MHz, e pelo Rádio Espectrômetro Solar Green Bank (GBSRBS) nas faixas de 100 - 300 MHz e 300 - 1200 MHz. A explosão solar apresenta uma estrutura temporal complexa em micro-ondas composta por três aumentos característicos. Explosões métricas e decamétricas tipo III foram acompanhadas por pequenas explosões com polarização em 45 e 90 GHz com graus de polarização de 0,09 e 0,12, sugerindo variações de campo magnético da ordem de 700 e 2000 G, respectivamente. O SST detectou uma explosão impulsiva e aumentos significativos de 10% no índice de cintilação de forma intermitente durante todo o evento. O tempo de lançamento da CME inferido por extrapolação das observações do coronógrafo LASCO ao limbo solar coincide aproximadamente com o instante do excesso de emissão e mudança do grau de polarização em 45 e 90 GHz, sugerindo que a CME tenha resultado de um transiente magnético ocasionando uma instabilidade que gerou as estruturas impulsivas subsequentes.

Title: Evolution of Interplanetary Coronal Mass Ejections Author: Andrii Lynnyk Department: Department of Surface and Plasma Science Supervisor: RNDr. Marek Vandas, DrSc. e-mail address: vandas@ig.cas.cz Abstract: This thesis deals with deformation of the Interplanetary Coronal Mass Ejections (ICMEs) and their sub-class Magnetic Clouds (MCs) during their propagation in the Solar Wind (SW). The statistical study of the expanded MCs has shown that expansion greatly affects the MC internal magnetic field. We had shown that this influence is more clear for the MCs observed close to their axes. The study of the stand-off shock distance in front of the supersonic ICME confirms a smooth deformation of the ICMEs along their path from the Sun into interplanetary space. We observed that this deformation is increasing with the velocity of the ICME. This study also confirmed the difference in sheaths that are created in front of expanding and non-expanding ICMEs. We found that velocity distribution inside the MC is not uniform and it has large fluctuations. We found that the MC cross-section is usually strongly deformed. Keywords: interplanetary coronal mass ejection, magnetic cloud, magnetosheath, flux rope, magnetic field, shock, fitting

Made available in DSpace on 2016-03-15T19:35:57Z (GMT). No. of bitstreams: 1 Edith Tueros Cuadros.pdf: 4357925 bytes, checksum: 7a9a7c9700e9ab1b8e24a65ab089b198 (MD5) Previous issue date: 2016-02-02 / Fundação de Amparo a Pesquisa do Estado de São Paulo / Cosmic rays are strongly influenced by solar, geomagnetic and atmospheric phenomena. CARPET detector, conceived for cosmic rays observation with energies in the range between 105 - 1012 eV, is an important tool for the study of these phenomena. The Earth s atmosphere conditions are also affected by changes in the cosmic rays flux, therefore, cosmic rays characterization is important to define physical and chemical conditions of our atmosphere. To characterize the cosmic rays flux variations, detected on the ground, prior elimination of atmospheric pressure and temperature effects on ground level is needed, thus, data recorded by meteorological instruments on CASLEO were used for that corrections. To eliminate the effect of temperature through the whole vertical atmosphere it was applied the integral and the mass-average temperature method by using vertical temperature profiles. Both methods were tested using CARPET-TEL data for the year 2009, this data were previously corrected by pressure influences. The mass-average temperature method shows a better response when comparing the corrected CARPET date with neutron monitor observations .The whole cosmic rays flux data analysis, for CARPET-TEL data corrected by integral method (for the period 2006/04/01 - 2014/06/30), shows an anti-correlation with sunspot number and a clear seasonal variation after 2008. Two Forbush decreases (FD), were detected by CARPET which were produced by geo-effective CMEs. Both FD onsets coincided with the interplanetary shock instant, which preceded intense geomagnetic storms. With these results, we can reinforce that CARPET is an important tool to study long and short term cosmic rays behavior, because it has a similar response to experiments that operates at atmosphere particle energy ranges. / Os raios cósmicos são fortemente influenciados pelos fenômenos solares, geomagnéticos e atmosféricos. O detector CARPET, concebido para a observação dos raios cósmicos com energias na faixa compreendida entre 105 e 1012 eV, é uma ferramenta importante para o estudo desses fenômenos. As condições da nossa atmosfera são também afetadas pelas variações no fluxo de raios cósmicos que chegam a Terra, portanto sua caracterização é importante para se definir as condições físicas e químicas da mesma. Para caracterizar as variações do fluxo de raios cósmicos a partir de observações no solo é necessário a eliminação prévia da influência dos efeitos da pressão e temperatura atmosférica na superfície, para tal foram utilizados dados meteorológicos obtidos no CASLEO. Para a eliminação do efeito da temperatura ao longo de toda atmosfera foram utilizados o método integral e o método de temperatura ponderada pela massa que utilizam perfis verticais de temperatura. Os dois métodos foram testados para o ano de 2009 com os dados do canal TEL do CARPET previamente corrigidos pela pressão, sendo que o método de temperatura ponderada pela massa apresentou uma resposta melhor ao se comparar os dados corrigidos com os dados observados com monitores de nêutrons. A análise de todos os dados do fluxo raios cósmicos do canal TEL do CARPET (1/04/2006 a 30/06/2014) corrigidos pelo método integral, mostra a anti-correlação com o número de manchas solares, e uma variação sazonal pronunciada após 2008. Foram detectados dois decréscimos Forbush (FD) produzidos por CMEs geo-efetivos. O início de ambos FD coincidiu com o instante do choque interplanetário, que antecedeu tempestades geomagnéticas intensas. Com estes resultados reforçamos que o CARPET é uma ferramenta importante para estudo das modulações de raios cósmicos de longo e curto prazo porque apresenta uma resposta semelhante com os experimentos que fazem observações em outras faixas de energia.