The solar wind is a stream of charged particles flowing from the Sun, and it offers a unique way to study how energy moves through space. This flow is turbulent, meaning energy moves from large structures to smaller ones in a chaotic way. However, this process is not always smooth. Sometimes there are sudden, intense bursts like magnetic walls or sharp currents. These bursts, characterized by the loss of 'self-similarity', are known as intermittency and are essential for understanding how energy is transferred in space. In this study, we look at how intermittency changes as the solar wind travels away from the Sun. We use data from three spacecraft: Parker Solar Probe (PSP), Solar Orbiter (SolO), and Wind, which observe the solar wind at different distances. By comparing these observations, we can see how turbulence and energy loss behave near and far from the Sun. This helps us understand how the solar wind stays hot and how energy is transferred in the near-Earth space environment. These insights improve the models that scientists use to describe space weather and conditions throughout the solar system.