Coronal Mass Ejections (CMEs) are one of the primary manifestations of solar activity and represent a major source of Space Weather disturbances in the Earth's environment. These solar phenomena are a significant subject of study due to the complex processes they undergo from the moment they erupt from the solar corona and travel through the heliosphere, involving the intricate evolution and propagation of magnetized plasma and its identification at various heliocentric distances using different heliospheric missions. From an observational standpoint, techniques such as remote sensing and white-light observations via coronagraphs (e.g., SOHO and STEREO) allow for the tracking of the morphological evolution of CMEs. Additionally, in-situ observations from spacecraft located at different heliocentric distances, ranging from very close to the Sun, such as Parker Solar Probe and Solar Orbiter, to the Earth's vicinity, such as WIND and ACE, enable the tracking of specific regions within these structures. These measurements reveal key signatures such as flux ropes, shock fronts, and compression regions, which play a fundamental role in plasma dynamics and the modulation of energetic particles. On the other hand, analytical models are used to examine the physical mechanisms governing CME dynamics and their interaction with the ambient solar wind, as well as to estimate arrival times and provide accurate forecasts of potential CME impacts on Earth. By integrating multi-point observations with advanced numerical models, this talk offers a comprehensive view of the evolution and propagation of CMEs, while also discussing the primary current challenges in predicting their arrival time and their impact on the terrestrial space environment.