Effect of the latitudinal distribution of temperature at the coronal base on the interplanetary magnetic field configuration and the solar wind flow

2005 ◽  
Vol 110 (A12) ◽  
Author(s):  
Bo Li ◽  
Shadia Rifai Habbal ◽  
Xing Li ◽  
Chris Mountford
Keyword(s):  
Magnetic Field ◽  
Solar Wind ◽  
Interplanetary Magnetic Field ◽  
Field Configuration ◽  
Wind Flow ◽  
Latitudinal Distribution ◽  
Magnetic Field Configuration ◽  
Solar Wind Flow

Influence of the Interplanetary Magnetic Field on the Solar Wind Flow about Planetary Obstacles

2006 ◽  
Vol 122 (1-4) ◽  
pp. 209-219 ◽  
Author(s):  
Nikolai Erkaev ◽  
Alexander Mezentsev ◽  
Helfried Biernat
Keyword(s):  
Magnetic Field ◽  
Solar Wind ◽  
Interplanetary Magnetic Field ◽  
Wind Flow ◽  
Solar Wind Flow

scholarly journals APPLICATION OF A SOLAR WIND MODEL DRIVEN BY TURBULENCE DISSIPATION TO A 2D MAGNETIC FIELD CONFIGURATION

2014 ◽  
Vol 796 (2) ◽  
pp. 111 ◽  
Author(s):  
Roberto Lionello ◽  
Marco Velli ◽  
Cooper Downs ◽  
Jon A. Linker ◽  
Zoran Mikić
Keyword(s):  
Magnetic Field ◽  
Solar Wind ◽  
Field Configuration ◽  
Magnetic Field Configuration ◽  
Wind Model ◽  
Model Driven ◽  
Solar Wind Model

scholarly journals Reconstruction of geomagnetic activity and near-Earth interplanetary conditions over the past 167 yr – Part 2: A new reconstruction of the interplanetary magnetic field

2013 ◽  
Vol 31 (11) ◽  
pp. 1979-1992 ◽  
Author(s):  
M. Lockwood ◽  
L. Barnard ◽  
H. Nevanlinna ◽  
M. J. Owens ◽  
R. G. Harrison ◽  
...  
Keyword(s):  
Magnetic Field ◽  
Solar Wind ◽  
Interplanetary Magnetic Field ◽  
Geomagnetic Activity ◽  
Flow Speed ◽  
Range Data ◽  
Solar Wind Flow ◽  
Annual Means ◽  
Solar Wind Parameters ◽  
The Imf

Abstract. We present a new reconstruction of the interplanetary magnetic field (IMF, B) for 1846–2012 with a full analysis of errors, based on the homogeneously constructed IDV(1d) composite of geomagnetic activity presented in Part 1 (Lockwood et al., 2013a). Analysis of the dependence of the commonly used geomagnetic indices on solar wind parameters is presented which helps explain why annual means of interdiurnal range data, such as the new composite, depend only on the IMF with only a very weak influence of the solar wind flow speed. The best results are obtained using a polynomial (rather than a linear) fit of the form B = χ · (IDV(1d) − β)α with best-fit coefficients χ = 3.469, β = 1.393 nT, and α = 0.420. The results are contrasted with the reconstruction of the IMF since 1835 by Svalgaard and Cliver (2010).

Asymmetric shear flow effects on magnetic field configuration within oppositely directed solar wind reconnection exhausts

2009 ◽  
Vol 114 (A7) ◽  
pp. n/a-n/a ◽  
Author(s):  
S. Eriksson ◽  
J. T. Gosling ◽  
T. D. Phan ◽  
L. M. Blush ◽  
K. D. C. Simunac ◽  
...  
Keyword(s):  
Magnetic Field ◽  
Solar Wind ◽  
Shear Flow ◽  
Field Configuration ◽  
Magnetic Field Configuration ◽  
Flow Effects

scholarly journals MHD effects of the solar wind flow around planets

2000 ◽  
Vol 7 (3/4) ◽  
pp. 201-210 ◽  
Author(s):  
H. K. Biernat ◽  
N. V. Erkaev ◽  
C. J. Farrugia ◽  
D. F. Vogl ◽  
W. Schaffenberger
Keyword(s):  
Magnetic Field ◽  
Solar Wind ◽  
Mach Number ◽  
Boundary Conditions ◽  
Wind Flow ◽  
Magnetic Shear ◽  
Thermal Anisotropy ◽  
Terrestrial Magnetosphere ◽  
Solar Wind Flow

Abstract. The study of the interaction of the solar wind with magnetized and unmagnetized planets forms a central topic of space research. Focussing on planetary magnetosheaths, we review some major developments in this field. Magnetosheath structures depend crucially on the orientation of the interplanetary magnetic field, the solar wind Alfvén Mach number, the shape of the obstacle (axisymmetric/non-axisymmetric, etc.), the boundary conditions at the magnetopause (low/high magnetic shear), and the degree of thermal anisotropy of the plasma. We illustrate the cases of Earth, Jupiter and Venus. The terrestrial magnetosphere is axisymmetric and has been probed in-situ by many spacecraft. Jupiter's magnetosphere is highly non-axisymmetric. Furthermore, we study magnetohydrodynamic effects in the Venus magnetosheath.

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