The interaction of the solar wind termination shock with disturbances incident from the upstream solar wind is considered using a one-dimensional MHD (both transverse and oblique) model. This paper extends the work of Story and Zank [1995> (Paper 1) to include the effects of the interplanetary magnetic field. A decay law is derived to describe the damping of compound rarefaction/shock structures. The inclusion of a parallel magnetic field component leads to the production of slow-mode rarefactions and shocks. Therefore, depending on parameters, the interaction of the termination shock with interplanetary disturbances may serve to generate both slow- and fast-mode magnetosonic waves that propagate through the heliosheath. Furthermore, it follows from the simulations presented here that slow-mode waves and rotational discontinuities can be expected to occur, at least to some extent, at any region of the solar system where collisions between oblique MHD shocks occur. Some discussion regarding the relative local orientation of the heliospheric magnetic field, with respect to the interstellar magnetic field, is presented to address the possibility of a global rotational discontinuity(s) which may be necessary to connect the interplanetary magnetic field to the interstellar field. Some further results concerning the interaction of waves and shocks reflected from heliosheath structure with the termination shock are also presented.¿ 1997 American Geophysical Union