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Direct evidence of an inertial-range turbulent energy cascade has beenprovided by spacecraft observations in heliospheric plasmas. In the solar wind,the average value of the derived heating rate near 1 au is $\sim 10^{3}\,\mathrm{J\,kg^{-1}\,s^{-1}}$, an amount sufficient to account for observeddepartures from adiabatic expansion. Parker Solar Probe (PSP), even during itsfirst solar encounter, offers the first opportunity to compute, in a similarfashion, a fluid-scale energy decay rate, much closer to the solar corona thanany prior in-situ observations. Using the Politano-Pouquet third-order law andthe von K\'arm\'an decay law, we estimate the fluid-range energy transfer ratein the inner heliosphere, at heliocentric distance $R$ ranging from$54\,R_{\odot}$ (0.25 au) to $36\,R_{\odot}$ (0.17 au). The energy transferrate obtained near the first perihelion is about 100 times higher than theaverage value at 1 au. This dramatic increase in the heating rate isunprecedented in previous solar wind observations, including those from Helios,and the values are close to those obtained in the shocked plasma inside theterrestrial magnetosheath.

Enhanced Energy Transfer Rate in Solar Wind Turbulence Observed near the Sun from Parker Solar Probe