Solar wind energy flux observations in the inner heliosphere: first results from Parker Solar Probe

We investigate the solar wind energy flux in inner heliosphere using 12-day observations around each perihelion of Encounter One (E01), Two (E02), Four (E04), and Five (E05) Parker Solar Probe (PSP), respectively, with a minimum heliocentric distance 27.8 radii ($R_\odot{}$). Energy was calculated based on electron parameters (density $n_e$, core temperature $T_{c}$, suprathermal $T_{h}$) obtained from simplified analysis plasma quasi-thermal noise (QTN) spectrum measured by RFS/FIELDS bulk proton (bulk speed $V_p$ $T_p$) Faraday Cup onboard PSP, SPC/SWEAP. Combining E01, E02, E04, E05, averaged value normalized to 1 $R_\odot{}$ plus necessary overcome gravitation ($W_{R_\odot{}}$) is about 70$\pm$14 $W m^{-2}$, which similar average (79$\pm$18 m^{-2}$) derived Le Chat et al 24-year Helios, Ulysses, Wind at various distances heliolatitudes. It remarkable that distributions $W_{R_\odot{}}$ are nearly symmetrical well fitted Gaussians, much more so than AU, may imply small limits interactions transient structures.