Because direct measurements of the solar coronal magnetic field and plasma are extremely difficult and inaccurate, we use a modeling approach based on observational quantities, e.g. the measured photospheric magnetic field, to reconstruct the structure of the global solar corona. We compute the distribution of the magnetic field and the plasma in the global corona with a self-consistent magnetohydrostatic (MHS) model We take an analytic magnetohydrostatic model to extrapolate the magnetic field
in the corona from photospheric magnetic field measurement. In the model, the electric current density can be decomposed into two components: one component is aligned with the magnetic field lines, whereas the other component flows in spherical shells. The second component of the current produces finite Lorentz forces which are balanced by the pressure gradient and the gravity force. We derive the 3D distribution of the magnetic field
and plasma self-consistently in one model. The boundary conditions are given by a synoptic magnetogram on the inner boundary and by a source surface model at the outer boundary. The density in the model is higher in the
equatorial plane than in the polar region. We compare the magnetic field distribution of our model with potential and force-free field models for the same boundary conditions and find that our model differs noticeably from both. We discuss the application of the model
and how to improve the model

Authors: P. Ruan, T. Wiegelmann, B. Inhester, T. Neukirch, S. K. Solanki and L. Feng
Projects: Mount Wilson Observatory

Publication Status: in press
Last Modified: 2008-02-05 09:59