Comment on the paper ?solution of one-fluid model equations with short range retarding magnetic forces for the quiet solar wind? by Cuperman and Harten

1976 ◽  
Vol 40 (1) ◽  
pp. 35-38 ◽  
Author(s):  
Aaron Barnes
Keyword(s):  
Solar Wind ◽  
Short Range ◽  
Fluid Model ◽  
Magnetic Forces ◽  
Model Equations

A TWO-FLUID MODEL OF THE SOLAR WIND

1992 ◽  
pp. 95-98
Author(s):  
Ø. Sandbæk ◽  
E. Leer ◽  
T.E. Holzer
Keyword(s):  
Solar Wind ◽  
Fluid Model ◽  
Two Fluid Model ◽  
Two Fluid

Lattice Boltzmann Simulation of Two-Fluid Model Equations

2008 ◽  
Vol 47 (23) ◽  
pp. 9165-9173 ◽  
Author(s):  
Krishnan Sankaranarayanan ◽  
Sankaran Sundaresan
Keyword(s):  
Lattice Boltzmann ◽  
Fluid Model ◽  
Lattice Boltzmann Simulation ◽  
Two Fluid Model ◽  
Model Equations ◽  
Two Fluid

scholarly journals Three-dimensional multi-fluid model of a coronal streamer belt with a tilted magnetic dipole

2015 ◽  
Vol 33 (1) ◽  
pp. 47-53 ◽  
Author(s):  
L. Ofman ◽  
E. Provornikova ◽  
L. Abbo ◽  
S. Giordano
Keyword(s):  
Solar Wind ◽  
Heavy Ions ◽  
Fluid Model ◽  
Slow Solar Wind ◽  
Streamer Belt ◽  
Lower Corona ◽  
Adequate Model ◽  
Coronal Streamer ◽  
Ion Emission ◽  
D Model

Abstract. Observations of streamers in extreme ultraviolet (EUV) emission with SOHO/UVCS show dramatic differences in line profiles and latitudinal variations in heavy ion emission compared to hydrogen Ly-α emission. In order to use ion emission observations of streamers as the diagnostics of the slow solar wind properties, an adequate model of a streamer including heavy ions is required. We extended a previous 2.5-D multi-species magnetohydrodynamics (MHD) model of a coronal streamer to 3-D spherical geometry, and in the first approach we consider a tilted dipole configuration of the solar magnetic field. The aim of the present study is to test the 3-D results by comparing to previous 2.5-D model result for a 3-D case with moderate departure from azimuthal symmetry. The model includes O5+ ions with preferential empirical heating and allows for calculation of their density, velocity and temperature in coronal streamers. We present the first results of our 3-D multi-fluid model showing the parameters of protons, electrons and heavy ions (O5+) at the steady-state solar corona with a tilted steamer belt. We find that the 3-D results are in qualitative agreement with our previous 2.5-D model, and show longitudinal variation in the variables in accordance with the tilted streamer belt structure. Properties of heavy coronal ions obtained from the 3-D model together with EUV spectroscopic observations of streamers will help understanding the 3-D structures of streamers reducing line-of-sight integration ambiguities and identifying the sources of the slow solar wind in the lower corona. This leads to improved understanding of the physics of the slow solar wind.

Two-Fluid Model of the Solar Wind

1966 ◽  
Vol 16 (14) ◽  
pp. 628-631 ◽  
Author(s):  
P. A. Sturrock ◽  
R. E. Hartle
Keyword(s):  
Solar Wind ◽  
Fluid Model ◽  
Two Fluid Model ◽  
Two Fluid

scholarly journals Dispersive magnetized waves in the solar wind plasma

2010 ◽  
Vol 77 (3) ◽  
pp. 357-365 ◽  
Author(s):  
B. DASGUPTA ◽  
DASTGEER SHAIKH ◽  
P. K. SHUKLA
Keyword(s):  
Solar Wind ◽  
Dispersion Relation ◽  
Fluid Model ◽  
Phase Speed ◽  
Solar Wind Plasma ◽  
Small Scale ◽  
Linear Dispersion ◽  
Length Scales ◽  
Linear Dispersion Relation ◽  
Two Fluid Model

AbstractWe derive a generalized linear dispersion relation of waves in a strongly magnetized, compressible, homogeneous and isotropic quasi-neutral plasma. Starting from a two-fluid model, describing distinguishable electron and ion fluids, we obtain a six-order linear dispersion relation of magnetized waves that contains effects due to electron and ion inertia, finite plasma beta and angular dependence of phase speed. We investigate propagation characteristics of these magnetized waves in a regime where scale lengths are comparable with electron and ion inertial length scales. This regime corresponds essentially to the solar wind plasma, where length scales, comparable with ion cyclotron frequency, lead to dispersive effects. These scales in conjunction with linear waves present a great deal of challenges in understanding the high-frequency, small-scale dynamics of turbulent fluctuations in the solar wind plasma.

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