L F Burlaga (Laboratory for Extraterrestrial Physics, NASA Goddard Space Flight Center, Greenbelt, MD 20771; ph. 301-286-5956);

J Chen, R Santoro (Plasma Physics Division, Naval Research Laboratory, Washington, DC 20375; ph. 202-767-3134; e-mail: chen@ppdu.nrl.navy.mil)

We investigate the eruption and propagation of solar magnetic flux ropes that may be manifested as interplanetary magnetic clouds. A theoretical model is constructed in which the initial flux rope is below or above the solar equator. The velocity of the prescribed ambient solar wind is assumed to have latitudinal dependence and a non-radial component. The initial ``eruption'' velocity of the flux rope is allowed to have a north-south component. The momentum of the flux rope is coupled to the ambient flows through a drag term. We investigate the propagation of a range of initial flux ropes for various solar wind flow patterns and obtain the flux rope magnetic field, speed, and density at 1 AU. The results are compared with specific magnetic clouds including the January 10, 1997 event.