This document discusses the three-dimensional evolution of magnetic flux ropes ejected from the Sun as they propagate through the solar system. It notes that studying flux rope evolution requires a three-dimensional analysis and using multiple tools, including coronagraph observations of flux ropes in the lower corona, in-situ measurements as constraints, and modeling their propagation through the solar wind using MHD simulations. As flux ropes travel through the solar system, they experience deflection towards the equatorial plane and rotation towards the heliospheric current sheet due to kinematic interactions.