MAGNETIC CONFIGURATIONS OF RAY STRUCTURES OF THE SOLAR CORONA

An axially symmetrical model for the solar coronal ray is presented, i n which charged particles move on magnetic surfaces created by the cur rents localized in the vicinity of the photosphere. The simplest confi guration of the currents, necessary for construction of an adequate mo del, is a pair of co-axial currents of opposite direction, situated in the photospheric plane. Magnetic surfaces of such field contain a sep aratrix shaped like the helmet or the onion, which is pointed above ow ing to the saddle special point. Such structures of the solar coronal rays can be created by superposition of magnetic fields from a sunspot and a surrounding facula with the oppositely directed field. The temp erature profile along the coronal ray is qualitatively explained by co nservation of the adiabatic invariant in the drift motion theory of ch arged particles.