A method of self-consistent three-dimensional solution of the magnetohydrostatic equations using magnetogram data

Abstract

A technique is proposed for constructing three-dimensional solutions comlplying with the self-consistent magnetohydrostatic (MHS) equations and with observations along the line of sight of the magnetic field at the photosphere. The technique is a generalization of a paper Rudenko, {\tt arXiv:astro-ph/0004222} to a potential-field approximation. The solution of the problem under consideration leans a representation of the magnetic field in terms of a scalar function, with its subsequent harmonic expansion in terms of a spherical functional basis that satisfies specified boundary conditions. A numerical realization of the proposed method is expected to permit a real-time modelling of three-dimensional magnetic field, temperature, pressure and density distributions.

9 pages, uses kluwer.sty, submitted to Solar Phys

References in corpus (1)

• Extrapolation of the solar magnetic field within the potential-field approximation from full-disk magnetograms

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• Magnetic modelling and tomography: First steps towards a consistent reconstruction of the solar corona
• A Magnetostatic Grad-Rubin Code for Coronal Magnetic Field Extrapolations
• Three-dimensional analytical magnetohydrostatic equilibria of rigidly rotating magnetospheres in cylindrical geometry
• Three-Dimensional Solutions of the Magnetohydrostatic Equations For Rigidly Rotating Magnetospheres in Cylindrical Coordinates