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Artykuły w czasopismach na temat "Flashs des éruptions"
"CO2 Degassing relate to 2021 Nyiragongo Volcan éruption". Petroleum and Chemical Industry International 6, nr 1 (22.02.2023). http://dx.doi.org/10.33140/pcii.06.01.02.
Pełny tekst źródłaRozprawy doktorskie na temat "Flashs des éruptions"
Xing, Chen. "Le rôle de la reconnexion magnétique dans l'évolution des tubes de flux des éruptions solaires". Electronic Thesis or Diss., Université Paris sciences et lettres, 2023. http://www.theses.fr/2023UPSLO011.
Pełny tekst źródłaCoronal mass ejections (CMEs) are impulsive eruptions of plasmas in the solar corona. Their interaction with the Earth's magnetosphere can induce extreme space weather conditions, with a major impact on human activities related to advanced technologies. A thorough understanding of the evolution of CMEs and their progenitors is extremely important for predicting CME eruptions and their related space weather. In this thesis, using numerical simulations and space observations, we study the kinematics, thermal properties and magnetic field evolution of flux ropes in CME progenitors and CMEs, and especially, the specific role of magnetic reconnection. We have discovered that the initiation of CMEs before their impulsive rise is a multiple-physics coupled-process. We have shown that the initiation of CMEs is first triggered and driven by the reconnection in hyperbolic flux tubes, and then driven by the coupling of torus instability and reconnection. We have also shown that the hot channel before the impulsive ejection is built up by hot flux rope field lines, the latter of which are progressively formed and heated by slipping reconnection in thin current sheets surrounding the flux rope. We also studied the evolution of magnetic flux in CMEs, and found that the pre-eruptive flux rope, rather than the magnetic reconnection during the eruption, is most likely the main contributor to the toroidal flux of the CME. More specifically, the magnetic reconnection first increases and then decreases the toroidal flux of the CME flux rope during the eruption. In addition, we studied two new observational phenomena related to CMEs and flares in the solar lower atmosphere, which are manifestations of the growth and deformation of flux ropes in CME progenitors and CMEs induced by magnetic reconnection. Finally, we have proposed two methods for identifying the footpoints of flux ropes associated with CMEs, which will be very useful for future work aimed at studying their evolution in the solar corona and interplanetary space
Musset, Sophie. "Accélération et propagation des particules énergétiques dans la couronne solaire : de l'analyse des données de l'instrument RHESSI à la préparation de l'exploitation de l'instrument STIX sur Solar Orbiter". Thesis, Paris Sciences et Lettres (ComUE), 2016. http://www.theses.fr/2016PSLEO011/document.
Pełny tekst źródłaThe Sun is an active star and one manifestation of its activity is the production of solar flares. It is currently admitted that solar flares are caused by the release of magnetic energy during the process of magnetic reconnection in the solar upper atmosphere, the solar corona. During these flares, a large fraction of the magnetic energy is transferred to the acceleration of particles (electrons and ions). However, the details of particle acceleration during flares are still not completely understood.Several scenarios and models have been developed to explain particle acceleration. In some of them, electric fields, produced at the location of current sheets, which can be fragmented or collapsing, and which are preferentially located on quasi-separatrix layers (QSLs), are accelerating particles. To investigate a possible link between energetic particles and direct electric fields produced at current sheet locations, we looked for a correlation between X-ray emission from energetic electrons and electric currents which can be measured at the photospheric level. We used the Reuven Ramaty High Energy Solar Spectrometric Imager (RHESSI) data to produce spectra and images of the X-ray emissions during GOES X-class flares, and spectropolarimetric data from the Helioseismic and Magnetic Imager (HMI) onboard the Solar Dynamics Observatory (SDO) to calculate the vertical current densities from the reconstructed 3D vector magnetic field. A correlation between the coronal X-ray emissions (tracing the energetic electrons near the acceleration site) and the strong current ribbons at the photospheric level (tracing the coronal current sheet) was found in the five studied X-class flares. Moreover, thanks to the 12-minute time cadence of SDO/HMI, we could study for the first time the time evolution of electric currents: in several flares, a change in the current intensity, occurring during the flare peak, was found to be spatially correlated with X-ray emission sites. These observations enlighten a common evolution of both electric currents and X-ray emissions during the
Akramov, Tohir. "La reconnexion magnétique explosive dans les nappes de courant multiples : application à l'environnement des pulsars". Thesis, Strasbourg, 2017. http://www.theses.fr/2017STRAE012/document.
Pełny tekst źródłaThe Crab Nebula, containing in its center a highly magnetized neutron star - the Crab pulsar, was essentially considered as a standard steady-state candle in gamma rays. Recently, this point of view has been challenged by gamma-ray flares observed by space satellites AGILE/Fermi-LAT. Even if the relativistic magnetic wind of the pulsar is considered to be the source of energy, the physical mechanism underlying these eruptive events is still a mystery. In this thesis, we improved the understanding of a mechanism based on fast magnetic reconnection, starting from the model of the magnetic wind generated by the central pulsar which loses its rotational kinetic energy. Indeed, the structure of the magnetic wind implies the presence of stripes with magmatic field lines of alternating polarities (hence the name "striped wind") through the equatorial plane of the pulsar. In a simplified local model, we assume the initiation of the dynamics from a double-current sheet configuration (induced by the magnetic structure) in the striped wind reference
Thibeault, Christian. "Prédiction des éruptions solaires par assimilation de données avec les modèles d’avalanches". Thesis, 2020. http://hdl.handle.net/1866/24379.
Pełny tekst źródłaSolar flares are sudden releases of electromagnetic radiation, relativistic particles and occasionally coronal mass, caused by the release of magnetic energy from the solar corona. They pose a danger to astronauts in high orbits and directly impact the Earth, including significant disturbances on GPS systems, and can even cause damage to technological infrastructures, including electrical networks. Predicting solar flares is therefore considered to be one of the most critical challenges in space weather. However, no method presented in the literature can produce reliable predictions, highlighting the complex nature of the triggering of solar flares. We, therefore, present in this thesis an alternative method to the usual statistical forecasting techniques. Our method is based on data assimilation coupled with computationally inexpensive cellular automaton models called avalanche models. Avalanche models are a drastic simplification of the physics underlying the triggering of solar flares. Despite their simplicity, they reproduce reasonably well the long-term statistics of solar flares sizes. In this thesis, we present empirical analyses of the predictive capabilities of four models: the Lu and Hamilton (LH) model (Lu & Hamilton, 1991, ApJ, 412, 841-852), two deterministic-driven (D) models (Strugarek & Charbonneau, 2014, SoPh, 289(8), 2993-3015) and finally two models using the principle of minimum energy during magnetic reconnection, called DMC models, which are strongly inspired by the models presented by Farhang et al. (2018, ApJ, 859(1), 41). The DMC models were developed during this project; therefore, a chapter of this thesis is dedicated to their presentation and more detailed analyses of their characteristics. We show that for D and DMC models, a memory exists between large simulated events, despite the high stochasticity present within each of these models. We finally present in this thesis a new protocol for predicting solar flares, using data assimilation coupled with avalanche models. Our protocol is based on a simulated annealing method to adjust the initial condition of the model until it satisfactorily reproduces a series of observed events. Once this optimal initial condition is found, the resulting simulation produces our prediction. In this thesis, we show our algorithm's success in assimilating hundreds of synthetic observations (produced by the avalanche models themselves).
Morales, Laura F. "A new avalanche model for solar flares". Thèse, 2008. http://hdl.handle.net/1866/6406.
Pełny tekst źródłaKsiążki na temat "Flashs des éruptions"
R, Ramaty, Mandzhavidze Natalie i Hua Xin-Min 1945-, red. High energy solar physics: Greenbelt, MD, August 16-18, 1995. Woodbury, N.Y: AIP Press, 1996.
Znajdź pełny tekst źródłaR, Ramaty, Mandzhavidze Natalie, Hua Xin-Min 1945- i High Energy Solar Physics Workshop (1995 : Goddard Space Flight Center), red. High energy solar physics: Greenbelt, MD, August 16-18, 1995. Woodbury, N.Y: AIP Press, 1996.
Znajdź pełny tekst źródła(Editor), Rouven Ramaty, Natalie Mandzhavidze (Editor) i Xin-Min Hus (Editor), red. High-Energy Solar Physics (AIP Conference Proceedings). American Institute of Physics, 1998.
Znajdź pełny tekst źródła