Contribution à la comréhension du magnetisme solaire
| Item type | Current location | Call number | Copy number | Status | Date due | Barcode |
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Memoire
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Bibliothèque Centrale | 538.3 HAB.2018 (Browse shelf) | 1 | Not For Loan | 5010000321024 | |
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Memoire
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Bibliothèque Centrale | 538.3 HAB.2018 (Browse shelf) | 2 | Not For Loan | 5010000321031 |
Mémoire présenté et défendu publiquement en vue de l'obtention du grade de licencié en pédagogie Appliquée, Agrégé de l'Enseignement secondaire en Physique
RÉSUME,
Solar magnetism is and remains an important subject for debate in many scientific circles. The Sun is generally an ionized plasma, governed by the convection movements of charged particles and differential rotation of all its constituents. Its magnetic field originates in the interface between the radiative and convective zones called tachocline. In this star of the day,this magnetic field is generated by the dyammo effect. this effect produces two components. the toroidal and the other poloidal, the latter regenerating from the other by the alpha effect, the opposite phonomenon being the omega effect. The alpha effect known as Rayleigh-Tayalorinstability is responsible for the oscillations of the solar magnetic field. This oscillation of the alpha effect is triggered approximately every 11 years, probably due to the alignment between the sun, the Earth, Venus and Jupiter, to cause the reseversal of polarity of the solar magnetic field, finally dictating the cycle of 22 years of the solar dynamo. The omega effect originates from the tachocline in which different zones of rotation converge, this phenomenon generates two magnetic bands located in the north-south axis of its equator. The origin of the solar magnetic field is not completely understood and only the thery of solar dynamo remains the currently most accepted mlechanism. The activity of this magnetic field directly depends on all phenomena observed onthe surface of the sun such as sunspots or eruptions as well as protuberances and ejections of coronal masses.
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