  Turbulence is a chaotic flow regime filled by irregular flows. The
dissipation of turbulence is a fundamental problem in the realm of physics.
Theoretically, dissipation cannot be ultimately achieved without collisions,
and so how turbulent kinetic energy is dissipated in the nearly collisionless
solar wind is a challenging problem. Wave particle interactions and magnetic
reconnection are two possible dissipation mechanisms, but which mechanism
dominates is still a controversial topic. Here we analyze the dissipation
region scaling around a solar wind magnetic reconnection region. We find that
the magnetic reconnection region shows a unique multifractal scaling in the
dissipation range, while the ambient solar wind turbulence reveals a
monofractal dissipation process for most of the time. These results provide the
first observational evidences for the intermittent multifractal dissipation
region scaling around a magnetic reconnection site, and they also have
significant implications for the fundamental energy dissipation process.
