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The Evolution of the 1/f Range within a Single Fast-solar-wind Stream between 17.4 and 45.7 Solar Radii

AuthorDavis, Nooshin; Chandran, B.~D.~G.; Bowen, T.~A.; Badman, S.~T.; de Wit, Dudok; Chen, C.~H.~K.; Bale, S.~D.; Huang, Zesen; Sioulas, Nikos; Velli, Marco;
KeywordsParker Data Used; Magnetohydrodynamics; Solar wind; interplanetary turbulence; 1964; 1534; 830; Astrophysics - Solar and Stellar Astrophysics; Physics - Space Physics
AbstractThe power spectrum of magnetic field fluctuations in the fast solar wind (V $_SW$ > 500 km s$^-1$) at magnetohydrodynamic scales is characterized by two different power laws on either side of a break frequency f $_b$. The low-frequency range at frequencies f smaller than f $_b$ is often viewed as the energy reservoir that feeds the turbulent cascade at f > f $_b$. At heliocentric distances r exceeding 60 solar radii (R $_s$), the power spectrum often has a 1/f scaling at f < f $_b$, i.e., the spectral index is close to -1. In this study, measurements from the Parker Solar Probe s Encounter 10 with the Sun are used to investigate the evolution of the magnetic field power spectrum at f < f $_b$ at r < 60 R $_s$ during a fast radial scan of a single fast-solar-wind stream. We find that the spectral index in the low-frequency part of the spectrum decreases from approximately -0.61 to -0.94 as r increases from 17.4 to 45.7 R $_s$. Our results suggest that the 1/f spectrum that is often seen at large r in the fast solar wind is not produced at the Sun, but instead develops dynamically as the wind expands outward from the corona into the interplanetary medium.
Year of Publication2023
Number of Pages154
Date Publishedjun