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Magnetic fielos and dynamos in space ano astrophysical plasmas

Abstract

The magnetic fields observed in stars and galaxies display magnetic energy comparable to the kinetic energy of the fluids where they are embedded. This is due to the presence of dynamo mechanisms, whereby the kinetic energy is converted into magnetic energy. Oynamos and magnetic fields play a crucial role in the solar variability, with direct impact on the Earth's climate. Moreover, magnetic fields are important for the magnetorotational instability, which is responsible for the generation of turbulence in accretion disks. Such turbulence is necessary for the outward transport of angular momentum, enabling the accretion of matter to the central object and consequently, the formation of stars and planets. This project proposes the simulation and analysis of the nonlinear dynamics of magnetic fields in space and astrophysical plasmas by means of the numerical solution of the magnetohydrodynamics (MHO) equations. The MHO equations will be solved for different values of the control parameters and boundary conditions, aiming the study of transition to turbulence in accretion disks, magnetic field quenching in the solar dynamo, and transport of passive scalars in magnetoconvection. To make simulations feasible, we propose the assembling of a high-performance computing laboratory, which will be available to a network of national and international collaborators. (AU)

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Scientific publications
(References retrieved automatically from Web of Science and SciELO through information on FAPESP grants and their corresponding numbers as mentioned in the publications by the authors)
TOLEDO, B. A.; CHIAN, A. C. -L.; REMPEL, E. L.; MIRANDA, R. A.; MUNOZ, P. R.; VALDIVIA, J. A. Wavelet-based multifractal analysis of nonlinear time series: The earthquake-driven tsunami of 27 February 2010 in Chile. Physical Review E, v. 87, n. 2 FEB 28 2013. Web of Science Citations: 10.

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