Applicability of Taylor's Hypothesis during Parker Solar Probe perihelia

Abstract

We investigate the validity of Taylor's Hypothesis (TH) in the analysis of Alfvénic fluctuations of velocity and magnetic fields in solar wind streams measured by Parker Solar Probe (PSP)~during the first four encounters. We use PSP velocity and magnetic field measurements from 24 h intervals selected from each of the first four encounters. The applicability of TH is investigated by measuring the parameter $\epsilon =\delta u_0/\sqrt{2}{V}_{\perp }$, which quantifies the ratio between the typical speed of large-scale fluctuations, $\delta u_0$, and the local perpendicular PSP speed in the solar wind frame, $V_{\perp }$. TH is expected to be applicable for $\epsilon \lesssim 0.5$ when PSP is moving nearly perpendicular to the local magnetic field in the plasma frame, irrespective of the Alfvén Mach number $M_{\mathrm{A}}=V_{\mathrm{SW}}/V_{\mathrm{A}}$, where $V_{\mathrm{SW}}$ and $V_{\mathrm{A}}$ are the local solar wind and Alfvén speed, respectively. For the four selected solar wind intervals we find that between 10% to 60% of the time the parameter $\epsilon$ is below 0.2 when the sampling angle (between the spacecraft velocity in the plasma frame and the local magnetic field) is greater than $30^{\circ }$. For angles above $30^{\circ }$, the sampling direction is sufficiently oblique to allow one to reconstruct the reduced energy spectrum $E(k_{\perp })$ of magnetic fluctuations from its measured frequency spectra. The spectral indices determined from power-law fits of the measured frequency spectrum accurately represent the spectral indices associated with the underlying spatial spectrum of turbulent fluctuations in the plasma frame. Aside from a frequency broadening due to large-scale sweeping that requires careful consideration, the spatial spectrum can be recovered to obtain the distribution of fluctuation's energy among scales in the plasma frame.

8 pages, 4 figures, submitted to Astronomy and Astrophysics

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• New Observations of Solar Wind 1/f Turbulence Spectrum from Parker Solar Probe
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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
• On the evolution of the Anisotropic Scaling of Magnetohydrodynamic Turbulence in the Inner Heliosphere
• Markovian Features of the Solar Wind at Sub-Proton Scales
• Galactic Cosmic-Ray Propagation in the Inner Heliosphere: Improved Force-Field Model
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• Dominance of 2-Minute Oscillations near the Alfvén Surface
• Taylor's Frozen-in Hypothesis for Magnetohydrodynamic turbulence and Solar Wind
• Solar Wind Structures from the Gaussianity of Magnetic Magnitude
• On the Interpretation of the Scalings of Density Fluctuations from In-situ Solar Wind Observations: Insights from 3D Turbulence Simulations
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