Modeling the Magnetic Field of the Inner Corona in a Radially Expanding Solar Wind

The magnetic field in the interplanetary medium is formed by action of sources on photosphere Sun and currents expanding atmosphere solar wind. In turn, high-speed plasma flow changes configuration lines. problem determining parameters near thus a three-dimensional interaction We present analytical expressions for calculating total vector B→(r, θ, ϕ) (in spherical coordinates) radially wind finite conductivity. are given form dimensionless Reynolds number as an arbitrary function radius, r: Rm = rσμv=ξ(r), where σ, μ, v denote, respectively, conductivity, permeability, velocity solution components obtained decomposition functions radial part depending distance from Sun. Examples calculations fields structures corona eclipse 21 August 2017 given.