Simulação MHD Bi-Dimensional da interação do vento solar com magnetosferas planetárias / Two-dimensional MHD simulation of the solar wind and planetary magnetospheres interaction

AUTOR(ES)
DATA DE PUBLICAÇÃO

2006

RESUMO

Space weather refers to conditions on the Sun and solar wind, magnetosphere and ionosphere that can influence the performance and reliability of ground-based technological systems and can aect the human life and health. The study of magnetospheres is of great scientific interest because it provides ideal laboratories to study the behavior of plasmas. The size of the magnetosphere is determined by the balance between the solar wind dynamic pressure and the pressure exerted by the magnetosphere, principally that of its magnetic field. The shape of the magnetosphere is additionally influenced by the drag of the solar wind, or tangential stress, on it. This drag is predominantly caused by the mechanism known as magnetic reconnection in which the magnetic field of the solar wind links to the magnetic field of the magnetosphere. This interaction between solar wind and planetary magnetospheres is not easily understood from the measurements limited by spacecrafts trajectories which make that heliosphere and magnetosphere, vast regions of space, have relatively few in situ measurements. The global magnetohidrodynamic (MHD) model, developed to solve for the magnetospheric configuration and to provide a self-consistent picture of the solar wind-magnetosphere interaction process, has been successful used for the past decades. The MHD theory deals with the macroscopic energy conversion governing the global configuration, that is, the physical processes involved in the conversion among the magnetic, kinetic and thermal energy. In this work, we used a two-dimensional MHD model to investigate the formation of the magnetosphere for diferent conditions of dipolar inclination (0, 45 or 90). In each case of dipolar inclination the IMF was changed to null, northward or southward. The original code of T. Ogino (1986) was modified to adjust the study purposes. This changes were coherent when the results were compared with other works in the literatute. Moreover, pression and current configurations over time were obtained and describe the characteristics of the solar wind-magnetosphere interaction. The velocity of the solar wind was modified to null inclination and IMF conditions and the relation between solar wind velocity and plasma sheet density was checked.

ASSUNTO(S)

geofÍsica espacial simulação magnetohidrodinâmica interação solar planetária magnetosferas planetárias geofísica vento solar space geophysics magnetohidrodynamic simulation solar planetary interaction planetary magnetospheres geophysics solar wind

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