scholarly journals Radial Density Distribution in the Plasma Column in the Region of the Critical Magnetic Field

1962 ◽  
Vol 28 (3) ◽  
pp. 562-564 ◽  
Author(s):  
Masatomo Sato
Keyword(s):  
Magnetic Field ◽  
Density Distribution ◽  
Plasma Column ◽  
Critical Magnetic Field ◽  
Radial Density ◽  
Radial Density Distribution

Diffusion eines Plasmas in Abhängigkeit von Magnetfeld und Drude und von der Längs-Ausdehnung in Magnetfeldrichtung

1963 ◽  
Vol 18 (8-9) ◽  
pp. 889-895
Author(s):  
F. Schwirzke
Keyword(s):  
Magnetic Field ◽  
Density Profile ◽  
Plasma Column ◽  
Uniform Magnetic Field ◽  
Radial Density ◽  
Radial Density Profile ◽  
Radial Density Distribution ◽  
Field Lines ◽  
Different Gases ◽  
The Magnetic Field

The radial density distribution for a plasma in a uniform magnetic field was studied in dependence of pressure and distance of the conducting end plates. It was possible to confirm experimentally the dependence of the radial distribution of the finite length in direction of the field lines. The influence of the magnetic field, of the pressure, and of the length of the plasma column on the radial density profile is, in different gases, qualitatively in accordance with the “short-circuiting” theory of A. SIMON.

Radial Density Distribution and Field Fluctuation of Magnetized Positive Column in Turbulence

1970 ◽  
Vol 29 (5) ◽  
pp. 1397-1397 ◽  
Author(s):  
Takeshi Takashima ◽  
Hiroshi Sato ◽  
Michio Matsumoto ◽  
Yoshiei Nakano
Keyword(s):  
Density Distribution ◽  
Positive Column ◽  
Radial Density ◽  
Field Fluctuation ◽  
Radial Density Distribution

scholarly journals Calculation of Radial Density Distribution Function for main orbital of Carbon atom and Carbon like ions

2014 ◽  
Vol 11 (4) ◽  
pp. 1455-1458
Author(s):  
Baghdad Science Journal
Keyword(s):  
Distribution Function ◽  
Carbon Atom ◽  
Density Distribution ◽  
Computer Software ◽  
Negative Ion ◽  
Radial Density ◽  
Density Distribution Function ◽  
Hartree Fock ◽  
Radial Density Distribution ◽  
Nitrogen Ion

Radial density distribution function of one particle D(r1) was calculated for main orbital of carbon atom and carbon like ions (N+ and B- ) by using the Partitioning technique .The results presented for K and L shells for the Carbon atom and negative ion of Boron and positive ion for nitrogen ion . We observed that as atomic number increases the probability of existence of electrons near the nucleus increases and the maximum of the location r1 decreases. In this research the Hartree-fock wavefunctions have been computed using Mathcad computer software .

Fragmentation of a Filamentary Cloud Threaded by Perpendicular Magnetic Field

2018 ◽  
Vol 14 (A30) ◽  
pp. 105-105
Author(s):  
Tomoyuki Hanawa ◽  
Takahiro Kudoh ◽  
Kohji Tomisaka
Keyword(s):  
Magnetic Field ◽  
Magnetic Force ◽  
Outer Boundary ◽  
Radial Distance ◽  
Radial Density ◽  
Radial Density Distribution ◽  
Model Cloud ◽  
Moderate Magnetic Field ◽  
Self Gravity ◽  
The Magnetic Field

AbstractFilamentary molecular clouds are thought to fragment to form clumps and cores. However, the fragmentation may be suppressed by magnetic force if the magnetic fields run perpendicularly to the cloud axis. We evaluate the effect using a simple model. Our model cloud is assumed to have a Plummer like radial density distribution, $\rho = {\rho _{\rm{c}}}{\left[ {1 + {r^2}/(2p{H^2})} \right]^{2p}}$ , where r and H denote the radial distance from the cloud axis and the scale length, respectively. The symbols, ρc and p denote the density on the axis and radial density index, respectively. The initial magnetic field is assumed to be uniform and perpendicular to the cloud axis. The model cloud is assumed to be supported against the self gravity by gas pressure and turbulence. We have obtained the growth rate of the fragmentation instability as a function of the wavelength, according to the method of Hanawa, Kudoh & Tomisaka (2017). The instability depends crucially on the outer boundary. If the displacement vanishes in regions very far from the cloud axis, cloud fragmentation is suppressed by a moderate magnetic field. If the displacement is constant along the magnetic field in regions very far from the cloud, the cloud is unstable even when the magnetic field is infinitely strong. The wavelength of the most unstable mode is longer for smaller index, p.

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