The knowledge of plasma pressure is essential for many physics applications in the magnetosphere, such as computing magnetospheric currents and deriving mag-netosphere-ionosphere coupling. A thorough knowledge of the 3-D pressure distribution has, however, eluded the community, as most in situ pressure observations are either in the ionosphere or the equatorial region of the magnetosphere. With the assumption of pressure isotropy there have been attempts to obtain the pressure at different locations,by either (a) mapping observed data (e.g. in the ionosphere) along the field lines of an empirical magnetospheric field model, or (b) computing a pressure profile in the equatorial plane (in 2-D) or along the Sun-Earth axis (in 1-D) th...
Two dimensional and three dimensional MHD equilibrium models were begun for Earth's magnetosphere. T...
[1] Localized reductions in the magnetic field associated with plasma pressure in Mercury’s magnetos...
Active regions (ARs) are typical magnetic structures found in the solar atmosphere. We calculate sev...
The knowledge of plasma pressure is essential for many physics applications in the magnetosphere, su...
Abstract. The knowledge of plasma pressure is essential for many physics applications in the magneto...
International audienceThe knowledge of plasma pressure is essential for many physics applications in...
The author presents the results of studies using magnetic field models and observations to determine...
In the absence of the toroidal flux, two coupled quasi two-dimensional elliptic equilibrium equation...
Abstract. Using the empirical magnetospheric magne-tic field models of Tsyganenko and Usmanov (TU), ...
A numerical procedure has been developed to deduce the plasma pressure and anisotropy from the Tsyg...
A numerical procedure has been developed to deduce the plasma pressure and anisotropy from the Tsyga...
Using the empirical magnetospheric magnetic field models of Tsyganenko and Usmanov (TU), we have det...
In this paper, we study whether the magnetic field of the T96 empirical model can be in force balanc...
Using the empirical magnetospheric magnetic field models of Tsyganenko and Usmanov (TU), we have det...
Empirical modeling of plasma pressure and magnetic field for the quiet time nightside magnetosphere ...
Two dimensional and three dimensional MHD equilibrium models were begun for Earth's magnetosphere. T...
[1] Localized reductions in the magnetic field associated with plasma pressure in Mercury’s magnetos...
Active regions (ARs) are typical magnetic structures found in the solar atmosphere. We calculate sev...
The knowledge of plasma pressure is essential for many physics applications in the magnetosphere, su...
Abstract. The knowledge of plasma pressure is essential for many physics applications in the magneto...
International audienceThe knowledge of plasma pressure is essential for many physics applications in...
The author presents the results of studies using magnetic field models and observations to determine...
In the absence of the toroidal flux, two coupled quasi two-dimensional elliptic equilibrium equation...
Abstract. Using the empirical magnetospheric magne-tic field models of Tsyganenko and Usmanov (TU), ...
A numerical procedure has been developed to deduce the plasma pressure and anisotropy from the Tsyg...
A numerical procedure has been developed to deduce the plasma pressure and anisotropy from the Tsyga...
Using the empirical magnetospheric magnetic field models of Tsyganenko and Usmanov (TU), we have det...
In this paper, we study whether the magnetic field of the T96 empirical model can be in force balanc...
Using the empirical magnetospheric magnetic field models of Tsyganenko and Usmanov (TU), we have det...
Empirical modeling of plasma pressure and magnetic field for the quiet time nightside magnetosphere ...
Two dimensional and three dimensional MHD equilibrium models were begun for Earth's magnetosphere. T...
[1] Localized reductions in the magnetic field associated with plasma pressure in Mercury’s magnetos...
Active regions (ARs) are typical magnetic structures found in the solar atmosphere. We calculate sev...