Contextual Predictions for Parker Solar Probe II: Turbulence Properties and Taylor Hypothesis

Abstract

The Parker Solar Probe (PSP) primary mission extends seven years and consists of 24 orbits of the Sun with descending perihelia culminating in a closest approach of ($\sim 9.8R_{\odot }$). In the course of these orbits PSP will pass through widely varying conditions, including anticipated large variations of turbulence properties such as energy density, correlation scales and cross helicities. Here we employ global magnetohydrodynamics simulations with self-consistent turbulence transport and heating \citep{usmanov2018} to preview likely conditions that will be encountered by PSP, by assuming suitable boundary conditions at the coronal base. The code evolves large-scale parameters -- such as velocity, magnetic field, and temperature -- as well as turbulent energy density, cross helicity, and correlation scale. These computed quantities provide the basis for evaluating additional useful parameters that are derivable from the primary model outputs. Here we illustrate one such possibility in which computed turbulence and large-scale parameters are used to evaluate the accuracy of the Taylor "frozen-in" hypothesis along the PSP trajectory. Apart from the immediate purpose of anticipating turbulence conditions that PSP will encounter, as experience is gained in comparisons of observations with simulated data, this approach will be increasingly useful for planning and interpretation of subsequent observations.

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Cited by in corpus (23)

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• Subproton-scale Intermittency in Near-Sun Solar Wind Turbulence Observed by the Parker Solar Probe
• Clustering of Intermittent Magnetic and Flow Structures near Parker Solar Probe's First Perihelion -- A Partial-Variance-of-Increments Analysis
• The Radial Dependence of Proton-scale Magnetic Spectral Break in Slow Solar Wind during PSP Encounter 2
• Applicability of Taylor's Hypothesis during Parker Solar Probe perihelia
• Magnetic Field Line Random Walk and Solar Energetic Particle Path Lengths: Stochastic Theory and PSP/ISoIS Observation
• Large-scale Structure and Turbulence Transport in the Inner Solar Wind -- Comparison of Parker Solar Probe's First Five Orbits with a Global 3D Reynolds-averaged MHD Model
• The radial variation of the solar wind turbulence spectra near the kinetic break scale from Parker Solar Probe measurements
• An Extended and Fragmented Alfvén Zone in the Young Solar Wind
• Modeling Kelvin-Helmholtz instability-driven turbulence with hybrid simulations of Alfvénic turbulence
• The Evolution of the 1/f Range Within a Single Fast-Solar-Wind Stream Between 17.4 and 45.7 Solar Radii
• Modeling of Joint Parker Solar Probe - Metis/Solar Orbiter Observations
• Interpreting solar wind turbulent spectra beyond Taylor's Hypothesis
• Turbulent energization of electron power law tails during magnetic reconnection
• Anisotropic Magnetic Turbulence in the Inner Heliosphere -- Radial Evolution of Distributions observed by Parker Solar Probe
• An analytical model of turbulence in Parker spiral geometry and associated magnetic field line lengths
• Compressible Turbulence in the Near-Sun Solar Wind: Parker Solar Probe's First Eight Perihelia
• The effect of turbulence on the angular momentum of the solar wind
• Current sheets, plasmoids and flux ropes in the heliosphere. Part II: Theoretical aspects
• Magnetic Switchback Occurrence Rates in the Inner Heliosphere: Parker Solar Probe and 1 au
• Isotropization and Evolution of Energy-Containing Eddies in Solar Wind Turbulence: Parker Solar Probe, Helios 1, ACE, WIND, and Voyager 1