scholarly journals The Effect of Magnetic Turbulence Energy Spectra and Pickup Ions on the Heating of the Solar Wind

2010 ◽  
Author(s):  
C. S. Ng ◽  
A. Bhattacharjee ◽  
P. A. Isenberg ◽  
D. Munsi ◽  
C. W. Smith ◽  
...  
Keyword(s):  
Solar Wind ◽  
Energy Spectra ◽  
Turbulence Energy ◽  
Pickup Ions ◽  
Magnetic Turbulence

scholarly journals The Transport and Evolution of MHD Turbulence throughout the Heliosphere: Models and Observations

Fluids ◽  
2021 ◽  
Vol 6 (10) ◽  
pp. 368
Author(s):  
Laxman Adhikari ◽  
Gary P. Zank ◽  
Lingling Zhao
Keyword(s):  
Solar Wind ◽  
Magnetic Energy ◽  
Cosmic Ray ◽  
Residual Energy ◽  
Turbulence Energy ◽  
Asymmetric Distribution ◽  
Mhd Turbulence ◽  
Pickup Ions ◽  
Coulomb Collisions ◽  
Turbulence Transport

A detailed study of solar wind turbulence throughout the heliosphere in both the upwind and downwind directions is presented. We use an incompressible magnetohydrodynamic (MHD) turbulence model that includes the effects of electrons, the separation of turbulence energy into proton and electron heating, the electron heat flux, and Coulomb collisions between protons and electrons. We derive expressions for the turbulence cascade rate corresponding to the energy in forward and backward propagating modes, the fluctuating kinetic and magnetic energy, the normalized cross-helicity, and the normalized residual energy, and calculate the turbulence cascade rate from 0.17 to 75 au in the upwind and downwind directions. Finally, we use the turbulence transport models to derive cosmic ray (CR) parallel and perpendicular mean free paths (mfps) in the upwind and downwind heliocentric directions. We find that turbulence in the upwind and downwind directions is different, in part because of the asymmetric distribution of new born pickup ions in the two directions, which results in the CR mfps being different in the two directions. This is important for models that describe the modulation of cosmic rays by the solar wind.

Acceleration of interstellar pickup ions in the disturbed solar wind observed on Ulysses

1994 ◽  
Vol 99 (A9) ◽  
pp. 17637 ◽  
Author(s):  
G. Gloeckler ◽  
J. Geiss ◽  
E. C. Roelof ◽  
L. A. Fisk ◽  
F. M. Ipavich ◽  
...  
Keyword(s):  
Solar Wind ◽  
Pickup Ions

Large-scale Structure and Turbulence Transport in the Young Solar Wind – Comparison of Parker Solar Probe Observations with a Global 3D Reynolds-averaged MHD Model

2021 ◽  
Author(s):  
Rohit Chhiber ◽  
Arcadi Usmanov ◽  
William Matthaeus ◽  
Melvyn Goldstein ◽  
Riddhi Bandyopadhyay
Keyword(s):  
Solar Wind ◽  
Large Scale ◽  
Transport Equations ◽  
Turbulence Energy ◽  
Reynolds Stresses ◽  
Mean Flow ◽  
Coulomb Collisions ◽  
Flow Equations ◽  
Simulation Results ◽  
Turbulence Transport

<div>Simulation results from a global <span>magnetohydrodynamic</span> model of the solar corona and the solar wind are compared with Parker Solar <span>Probe's</span> (<span>PSP</span>) observations during its first several orbits. The fully three-dimensional model (<span>Usmanov</span> <span>et</span> <span>al</span>., 2018, <span>ApJ</span>, 865, 25) is based on Reynolds-averaged mean-flow equations coupled with turbulence transport equations. The model accounts for effects of electron heat conduction, Coulomb collisions, Reynolds stresses, and heating of protons and electrons via nonlinear turbulent cascade. Turbulence transport equations for turbulence energy, cross <span>helicity</span>, and correlation length are solved concurrently with the mean-flow equations. We specify boundary conditions at the coronal base using solar synoptic <span>magnetograms</span> and calculate plasma, magnetic field, and turbulence parameters along the <span>PSP</span> trajectory. We also accumulate data from all orbits considered, to obtain the trends observed as a function of heliocentric distance. Comparison of simulation results with <span>PSP</span> data show general agreement. Finally, we generate synthetic fluctuations constrained by the local rms turbulence amplitude given by the model, and compare properties of this synthetic turbulence with PSP observations.</div>

Spectral Exponents of Kinetic and Magnetic Energy Spectra in Solar Wind Turbulence

2007 ◽  
Vol 664 (1) ◽  
pp. 543-548 ◽  
Author(s):  
J. J. Podesta ◽  
D. A. Roberts ◽  
M. L. Goldstein
Keyword(s):  
Solar Wind ◽  
Magnetic Energy ◽  
Energy Spectra ◽  
Solar Wind Turbulence ◽  
Wind Turbulence

Inner Source C+/O+ Pickup Ions Produced by Solar Wind Recycling, Neutralization, Backscattering, Sputtering, and Sputtering-induced Recycling

2018 ◽  
Vol 861 (2) ◽  
pp. 98 ◽  
Author(s):  
P. R. Quinn ◽  
N. A. Schwadron ◽  
E. Möbius ◽  
A. Taut ◽  
L. Berger
Keyword(s):  
Solar Wind ◽  
Pickup Ions

Dependence of Pc 3 magnetic energy spectra at south pole on upstream solar wind parameters

1987 ◽  
Vol 92 (A11) ◽  
pp. 12437 ◽  
Author(s):  
K. Yumoto ◽  
A. Wolfe ◽  
T. Terasawa ◽  
E. L. Kamen ◽  
L. J. Lanzerotti
Keyword(s):  
Solar Wind ◽  
Magnetic Energy ◽  
Energy Spectra ◽  
South Pole ◽  
Solar Wind Parameters ◽  
Upstream Solar Wind

Thermal anisotropies in the solar wind: Evidence of heating by interstellar pickup ions?

1996 ◽  
Vol 23 (22) ◽  
pp. 3259-3262 ◽  
Author(s):  
John D. Richardson ◽  
John L. Phillips ◽  
Charles W. Smith ◽  
Perry C. Gray
Keyword(s):  
Solar Wind ◽  
Pickup Ions
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