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The scaling of the turbulent spectra provides a key measurement that allowsto discriminate between different theoretical predictions of turbulence. In thesolar wind, this has driven a large number of studies dedicated to this issueusing in-situ data from various orbiting spacecraft. While a semblance ofconsensus exists regarding the scaling in the MHD and dispersive ranges, theprecise scaling in the transition range and the actual physical mechanisms thatcontrol it remain open questions. Using the high-resolution data in the innerheliosphere from Parker Solar Probe (PSP) mission, we find that the sub-ionscales (i.e., at the frequency f ~ [2, 9] Hz) follow a power-law spectrum f^awith a spectral index a varying between -3 and -5.7. Our results also show thatthere is a trend toward and anti-correlation between the spectral slopes andthe power amplitudes at the MHD scales, in agreement with previous studies: thehigher the power amplitude the steeper the spectrum at sub-ion scales. Asimilar trend toward an anti-correlation between steep spectra and increasingnormalized cross helicity is found, in agreement with previous theoreticalpredictions about the imbalanced solar wind. We discuss the ubiquitous natureof the ion transition range in solar wind turbulence in the inner heliosphere.

The Ion Transition Range of Solar Wind Turbulence in the Inner Heliosphere: Parker Solar Probe Observations