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In this Letter we propose a practical methodology to interpret future Parker Solar Probe (PSP) turbulent time signals even when Taylor's hypothesis is not valid. By extending Kraichnan's sweeping model used in hydrodynamics we derive the Eulerian spacetime correlation function in magnetohydrodynamic (MHD) turbulence. It is shown that in MHD, the temporal decorrelation of small-scale fluctuations arises from a combination of hydrodynamic sweeping induced by large-scale fluid velocity delta u(0) and by the Alfvenic propagation along the local magnetic field. The resulting temporal part of the spacetime correlation function is used to determine the field-perpendicular wavenumber range Delta k(perpendicular to) = [k(min, )k(max)]of the turbulent fluctuations that contribute to the power of a given frequency omega of the time signal measured in the spacecraft frame. Our analysis also shows that the shape of frequency power spectrum P-sc(omega) of the time signal will follow the same power law of the reduced power spectrum E (k(perpendicular to)) similar to k(perpendicular to)(-alpha) in the plasma frame, where alpha is the spectral index. The proposed framework for the analysis of PSP time signals entirely relies on two simple dimensionless parameters that can be empirically obtained from PSP measurements, namely, epsilon = delta u(0)/root 2V(perpendicular to) (where V-perpendicular to is the perpendicular velocity of PSP seen in the plasma frame) and the spectral index alpha.

@article{Bourouaine2019, title = {On the interpretation of parker solar probe turbulent signals}, volume = {879}, issn = {2041-8205}, url = {https://doi.org/10.3847/2041-8213/ab288a}, doi = {10.3847/2041-8213/ab288a}, abstract = {In this Letter we propose a practical methodology to interpret future Parker Solar Probe (PSP) turbulent time signals even when Taylor's hypothesis is not valid. By extending Kraichnan's sweeping model used in hydrodynamics we derive the Eulerian spacetime correlation function in magnetohydrodynamic (MHD) turbulence. It is shown that in MHD, the temporal decorrelation of small-scale fluctuations arises from a combination of hydrodynamic sweeping induced by large-scale fluid velocity delta u(0) and by the Alfvenic propagation along the local magnetic field. The resulting temporal part of the spacetime correlation function is used to determine the field-perpendicular wavenumber range Delta k(perpendicular to) = [k(min, )k(max)]of the turbulent fluctuations that contribute to the power of a given frequency omega of the time signal measured in the spacecraft frame. Our analysis also shows that the shape of frequency power spectrum P-sc(omega) of the time signal will follow the same power law of the reduced power spectrum E (k(perpendicular to)) similar to k(perpendicular to)(-alpha) in the plasma frame, where alpha is the spectral index. The proposed framework for the analysis of PSP time signals entirely relies on two simple dimensionless parameters that can be empirically obtained from PSP measurements, namely, epsilon = delta u(0)/root 2V(perpendicular to) (where V-perpendicular to is the perpendicular velocity of PSP seen in the plasma frame) and the spectral index alpha.}, number = {1}, journal = {Astrophysical Journal Letters}, author = {Bourouaine, Sofiane and Perez, Jean C.}, year = {2019}, note = {Publisher: Iop Publishing Ltd Type: Article tex.date-modified: 2022-04-12 11:34:55 +0100}, }

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