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

摘要: Magnetic field fluctuations in the solar wind are commonly observed to follow a power law spectrum. Near proton-kinetic scales, spectral break occurs which is interpreted as transition kinetic turbulence. However, this not yet entirely understood. By studying scaling of with various plasma properties, it may be possible constrain processes leading onset Using data from Parker Solar Probe (\textit{PSP}), we measure proton scale over range heliocentric distances, enabling measurement inertial turbulence under conditions. We find that frequency $f_b$ increases distance $r$ decreases slow following $f_b\sim r^{-1.11}$. also compare characteristic ion scales relate physical mechanisms occurring at scale. The ratio between and $f_c$, Doppler shifted cyclotron resonance scale, approximately unity for all $\beta_p$. At high $\beta_p$ $f_\rho$, gyroscale, unity; while low $f_d$, proton-inertial length unity. Due large comparable Alfven speeds, analyze these results using both standard modified Taylor hypothesis, demonstrating robust statistical results.