Authors: Alexandros Chasapis (LASP), Y. Qi (LASP), T. Vo (LASP), R. Ergun (LASP), Trevor Bowen (SSL), L. Sorriso-Valvo (KTH), F. Pecora (University of Delaware), W. H. Matthaeus (University of Delaware), V. Montagud-Camps (Universidad de Murcia), E. Yordanova (IRF), I. Svenningsson (IRF), O. LeContel (LPP), A. Retino (LPP), M. Baraka (LPP)

Turbulence is a major pathway of energy exchange across the heliosphere. As the solar wind evolves out from the inner heliosphere, the turbulent cascade transfers energy to kinetic scales, leading to dissipation, plasma heating, and particle acceleration. Transient structures embedded in the solar wind such as CMEs and SIRs can significantly alter the local properties of the plasma and drive an enhancement of turbulent dissipation. Studying this link, and its impact on Earth’s magnetic environment, is crucial to our understanding of the Sun-Earth relationship. Observations by PSP and MMS allow us to trace the evolution of turbulence within such transient solar wind structures from the inner heliosphere to near-Earth space, where we observe a major enhancement of turbulent dissipation driven by the variable solar wind. We examine the evolution of the turbulent cascade, and the associated turbulent dissipation. We analyze the properties of the intermittent structures that form in the turbulence at kinetic scales, and their role in localized energy dissipation and particle energization.