A method to obtain uniform magnetic-field energy density gradient distribution using discrete pole pieces for a microelectromechanical-system-based magnetic cell separator

2006 ◽  
Vol 99 (8) ◽  
pp. 08R905 ◽  
Author(s):  
Pulak Nath ◽  
Lee R. Moore ◽  
Maciej Zborowski ◽  
Shuvo Roy ◽  
Aaron Fleischman
Keyword(s):  
Magnetic Field ◽  
Energy Density ◽  
Density Gradient ◽  
Uniform Magnetic Field ◽  
Field Energy ◽  
Microelectromechanical System ◽  
Gradient Distribution ◽  
Cell Separator ◽  
Magnetic Field Energy ◽  
Field Energy Density

scholarly journals Finite size scaling in the solar wind magnetic field energy density as seen by WIND

2002 ◽  
Vol 29 (10) ◽  
pp. 86-1-86-4 ◽  
Author(s):  
B. Hnat ◽  
S. C. Chapman ◽  
G. Rowlands ◽  
N. W. Watkins ◽  
W. M. Farrell
Keyword(s):  
Magnetic Field ◽  
Solar Wind ◽  
Energy Density ◽  
Finite Size ◽  
Field Energy ◽  
Finite Size Scaling ◽  
Size Scaling ◽  
Magnetic Field Energy ◽  
Solar Wind Magnetic Field ◽  
Field Energy Density

Variations in the ratio of particle to magnetic field energy density, as observed by Ulysses/HI-SCALE

1999 ◽  
Vol 24 (1-3) ◽  
pp. 79-81 ◽  
Author(s):  
G. Kasotakis ◽  
E.T. Sarris ◽  
P. Marhavilas ◽  
N. Sidiropoulos ◽  
P. Trochoutsos ◽  
...  
Keyword(s):  
Magnetic Field ◽  
Energy Density ◽  
Field Energy ◽  
Magnetic Field Energy ◽  
Field Energy Density

scholarly journals On the fractal nature of the magnetic field energy density in the solar wind

2007 ◽  
Vol 34 (15) ◽  
Author(s):  
B. Hnat ◽  
S. C. Chapman ◽  
K. Kiyani ◽  
G. Rowlands ◽  
N. W. Watkins
Keyword(s):  
Magnetic Field ◽  
Solar Wind ◽  
Energy Density ◽  
Field Energy ◽  
Fractal Nature ◽  
Magnetic Field Energy ◽  
Field Energy Density ◽  
The Magnetic Field

The interaction between a weak magnetic field and a black hole

1977 ◽  
Vol 356 (1686) ◽  
pp. 351-362 ◽  
Keyword(s):  
Magnetic Field ◽  
Black Hole ◽  
Angular Momentum ◽  
Asymptotic Form ◽  
Rotation Axis ◽  
Field Energy ◽  
Magnetic Field Energy ◽  
Teukolsky Equation ◽  
Field Energy Density ◽  
Component Parallel

The problem investigated is: what happens to a rotating black hole sunk in a vacuum magnetic field, constantly aligned at angle γ to its rotation axis far from the hole? The Newman-Penrose quantities Φ 0 and ρ -2 Φ 2 , which describe the radiation parts of the external field, are obtained as solutions to the Teukolsky equation with appropriate boundary conditions. From these two quantities the complete distant asymptotic form of the electromagnetic field is constructed via the four-vector potential A i , it by using the method of Chandrasekhar. Changes in the angular momentum of the hole are calculated. The component perpendicular to the field decreases exponentially with time according to the law J ⊥ = ( J ⊥ ) initial exp (- t ⊤ -1 ), Where ⊤ -1 =16/3 π G 2 c -5 (mass of hole) x (distant magnetic field energy-density), while the component parallel to the field remains constant. No energy emerges from the hole, kinetic rotational energy instead transforming into irreducible mass. This is precisely the outcome known from study of the slowly rotating hole. Extension of the result is of astrophysical relevance, since a real black hole may be rotating relatively fast. And it is of some theoretical interest that terms of second and higher order in angular momentum make no difference to the spin-down behaviour.

scholarly journals Generation of Magnetic Fields and Electric Currents in the Solar Photosphere

1990 ◽  
Vol 138 ◽  
pp. 273-277
Author(s):  
J.C. Henoux ◽  
B.V. Somov
Keyword(s):  
Magnetic Field ◽  
Radial Dependence ◽  
Field Energy ◽  
Solar Photosphere ◽  
Fluid Approximation ◽  
Flux Tubes ◽  
Magnetic Field Energy ◽  
Field Energy Density ◽  
Dc Current ◽  
The Magnetic Field

Velocities of electrons, ions and neutrals are computed in the three-fluid approximation for an axisymmetrical magnetic field. By prescribing a radial dependence of the velocity of neutrals in agreement with a downflow, the radial dependence of the magnetic field energy density is derived for a given set of values of the magnetic field at the central and external boundaries. Flux-tube cooling by advection of ionization energy is found to be significant. Vortices in the low photosphere could produce significant electric power and DC current intensity along the coronal magnetic lines of forces. The velocities of neutrals, the size and the number of flux-tubes required to power flares in plage regions, are estimated.

The interaction between a weak magnetic field and a slowly rotating black hole

1976 ◽  
Vol 350 (1661) ◽  
pp. 239-252 ◽  
Keyword(s):  
Magnetic Field ◽  
Boundary Condition ◽  
Black Hole ◽  
Angular Momentum ◽  
Rotation Axis ◽  
Homogeneous Magnetic Field ◽  
Field Energy ◽  
Rotating Black Hole ◽  
Magnetic Field Energy ◽  
Field Energy Density

We solve Maxwell’s equations in the vacuum space-time of the slowly rotating black hole (terms of second and higher order in angular momentum are ignored), with a homogeneous magnetic field aligned at angle γ to the rotation axis as boundary condition far from the hole, assuming that the field is always so weak as to have no influence upon the background metric. The solution is used to find the change of angular momentum of the hole. The component perpendicular to the field decreases exponentially with time according to the law J ⊥ = ( J ⊥ ) initial exp ( – t ז -1 ) where ז -1 = 1 6/3π G 2 c -5 (mass of hole) (magnetic field energy density at infinity), while the component parallel to the field remains constant. The axis of rotation of the black hole is thus caused to come into alignment with the magnetic field, although so gradually as to render remote the prospect of observational confirmation for any easily conceived astrophysical situation. With the chosen boundary condition on the field, no energy emerges from the hole, kinetic energy of rotation being transformed instead into irreducible mass.

COOLING OF RELATIVISTIC ELECTRONS IN TEV BLAZARS: CLUES FROM MULTIWAVELENGTH SPECTRA

2008 ◽  
Vol 17 (09) ◽  
pp. 1591-1601
Author(s):  
R. SCHLICKEISER
Keyword(s):  
Magnetic Field ◽  
Energy Density ◽  
Kinetic Energy ◽  
High Energy ◽  
Particle Energy ◽  
Field Energy ◽  
Kinetic Energy Density ◽  
Relativistic Electrons ◽  
Magnetic Field Energy ◽  
The Magnetic Field

In powerful cosmic nonthermal radiation sources with dominant magnetic-field self generation, the generation of magnetic fields at almost equipartition strength by relativistic plasma instabilities operates as fast as the acceleration or injection of ultra-high energy radiating electrons and hadrons in these sources. Consequently, the magnetic field strength becomes time-dependent and adjusts itself to the actual kinetic energy density of the radiating electrons in these sources. This coupling of the magnetic field and the magnetic field energy density to the kinetic energy of the radiating particles changes both the intrinsic temporal evolution of the relativistic particle energy spectrum after injection and the synchrotron and synchrotron self-Compton emissivities.

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