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Magnetic field fluctuations in the solar wind are commonly observed to followa power law spectrum. Near proton-kinetic scales, a spectral break occurs whichis commonly interpreted as a transition to kinetic turbulence. However, thistransition is not yet entirely understood. By studying the scaling of the breakwith various plasma properties, it may be possible to constrain the processesleading to the onset of kinetic turbulence. Using data from Parker Solar Probe(\textit{PSP}), we measure the proton scale break over a range of heliocentricdistances, enabling a measurement of the transition from inertial to kineticscale turbulence under various plasma conditions. We find that the breakfrequency $f_b$ increases as the heliocentric distance $r$ decreases in theslow solar wind following a power law $f_b\sim r^{-1.11}$. We also compare thisto the characteristic plasma ion scales to relate the break to the possiblephysical mechanisms occurring at this scale. The ratio between $f_b$ and $f_c$,the Doppler shifted ion cyclotron resonance scale, is approximately unity forall plasma $\beta_p$. At high $\beta_p$ the ratio between $f_b$ and $f_\rho$,the Doppler shifted gyroscale, is approximately unity; while at low $\beta_p$the ratio between $f_b$ and $f_d$, the Doppler shifted proton-inertial lengthis unity. Due to the large comparable Alfv\'en and solar wind speeds, weanalyze these results using both the standard and modified Taylor hypothesis,demonstrating robust statistical results.

The Radial Dependence of Proton-scale Magnetic Spectral Break in Slow Solar Wind during PSP Encounter 2