The determination of coronal potential magnetic fields using lineofsight boundary conditions
Abstract
Previous efforts to construct solar coronal fields using surface magnetograph data have generally employed a least squares minimization technique in order to determine the spherical harmonic expansion coefficients of the magnetic scalar potential. Provided there is no source surface high up in the corona, we show that knowledge of the lineofsight component of the surface magnetic field, B_{i} = B_{r} sin θ + B_{θ} cos θ, is sufficient to uniquely determine the potential coronal magnetic field by an explicit construction of the magnetic scalar potential for an arbitrary B_{l}(θ, φ).
 Publication:

Solar Physics
 Pub Date:
 February 1986
 DOI:
 10.1007/BF00147832
 Bibcode:
 1986SoPh..103..311B
 Keywords:

 Boundary Conditions;
 Boundary Value Problems;
 Line Of Sight;
 Solar Corona;
 Solar Magnetic Field;
 Potential Fields;
 Stellar Models;
 Solar Physics;
 Boundary Condition;
 Magnetic Field;
 Expansion Coefficient;
 Scalar Potential;
 Explicit Construction