SPATIAL PROFILES OF LINES IN STEADY-STATE CORONAL LOOPS

A steady-state model of the magnetically confined plasma in coronal loops is presented by expressing the magnetic field and fluid velocity in terms of a single Chandrasekhar-Kendall function. For the Chandrasekhar-Kendall function with n = 0 = m, we found a radial variation of pressure. For constant electron density, the temperature increases radially outwards. The variations of the fluxes for lines from CII, CIII, OIV, NeVII, and MgX along the radius of the loop are plotted. The hotter lines generated near the surface of the loop show larger spatial extents than the cooler lines emitted in the core of the loop, which is in agreement with observations.