A Two-Component Model of the Quiet Solar Wind with Viscosity, Magnetic Field, and Reduced Heat Conduction

1971 ◽  
Vol 165 ◽  
pp. 181 ◽  
Author(s):  
Charles L. Wolff ◽  
John C. Brandt ◽  
Robert G. Southwick
Keyword(s):  
Magnetic Field ◽  
Solar Wind ◽  
Heat Conduction ◽  
Component Model ◽  
Two Component

Galactic magnetic-field models derived from Faraday-rotation data

1967 ◽  
Vol 31 ◽  
pp. 391-392
Author(s):  
R. D. Davies
Keyword(s):  
Magnetic Field ◽  
Faraday Rotation ◽  
Component Model ◽  
The Sun ◽  
Galactic Magnetic Field ◽  
Two Component ◽  
Net Flux ◽  
The Magnetic Field ◽  
Disk Component ◽  
Spiral Arm

The distribution of rotation measures for 86 sources suggests a two-component model for the magnetic field: a disk component directed towardl= 95°, and a component in the local spiral arm, directed alongl= 70° and 250°, with opposite senses above and below the plane. The latter may be due to a looped field in a cloud surrounding the Sun; its net flux is 3·5 micro-gauss.

scholarly journals A GENERALIZED TWO-COMPONENT MODEL OF SOLAR WIND TURBULENCE AND AB INITIO DIFFUSION MEAN-FREE PATHS AND DRIFT LENGTHSCALES OF COSMIC RAYS

2016 ◽  
Vol 833 (1) ◽  
pp. 17 ◽  
Author(s):  
T. Wiengarten ◽  
S. Oughton ◽  
N. E. Engelbrecht ◽  
H. Fichtner ◽  
J. Kleimann ◽  
...  
Keyword(s):  
Solar Wind ◽  
Cosmic Rays ◽  
Ab Initio ◽  
Component Model ◽  
Solar Wind Turbulence ◽  
Two Component ◽  
Wind Turbulence

scholarly journals Interpretation of Some Properties of Extragalactic Jets in the Context of a Two Component Model

1994 ◽  
Vol 159 ◽  
pp. 433-433
Author(s):  
Lourdes Vicente
Keyword(s):  
Magnetic Field ◽  
Accretion Disk ◽  
Thermal Plasma ◽  
Slow Component ◽  
Critical Value ◽  
Component Model ◽  
Parallel Magnetic Field ◽  
Electron Positron ◽  
Extragalactic Jets ◽  
Two Component

We have studied a sample of extragalactic jets within the context of a two component model. This model supposes the existence of two flows in the extragalactic jets. An electron-positron fast beam coming from the internal regions of the accretion disk, responsible for the VLBI jet at the parsec scale and for the observed superluminal speeds. A second slow component, responsible for the jet observed at larger scales. The fast beam is destroyed when the parallel magnetic field is smaller than a critical value, BII < Bcrit = 3.2 × 10−3np1/2, where np is the density of the background thermal plasma of the slow component.

scholarly journals Transport of solar wind fluctuations: A two-component model

2011 ◽  
Vol 116 (A8) ◽  
pp. n/a-n/a ◽  
Author(s):  
S. Oughton ◽  
W. H. Matthaeus ◽  
C. W. Smith ◽  
B. Breech ◽  
P. A. Isenberg
Keyword(s):  
Solar Wind ◽  
Component Model ◽  
Two Component

scholarly journals Properties of Photospheric Fluxtubes Derived from Magnetograph Observations

1990 ◽  
Vol 138 ◽  
pp. 125-128
Author(s):  
V.G. Lozitskij ◽  
T.T. Tsap
Keyword(s):  
Magnetic Field ◽  
Field Strength ◽  
Spectral Line ◽  
Spatial Resolution ◽  
Background Field ◽  
Component Model ◽  
Ratio Method ◽  
Line Profiles ◽  
Two Component ◽  
The Magnetic Field

Data from magnetograph observations, obtained in six Fe I and Mg I lines with the Crimean magnetograph with a spatial resolution of 1 × 1 and 1 × 2 arcsec have been interpreted using the line-ratio method and a two-component model with spatially unresolved fluxtubes and a background field. Magnetograph data obtained by other authors have also been taken into account. The magnetic field strength, its variation with distance from the fluxtube axis, the characteristics of the spectral line profiles, as well as other properties of the fluxtubes have been determined.

H-Cmes and Ii-Type Radio Bursts Related Intense Geomagnetic Storms in Relation With Interplanetary Magnetic Field and Solar Wind Disturbances

2012 ◽  
Vol 2 (10) ◽  
pp. 1-3 ◽  
Author(s):  
Praveen Kumar Gupta ◽  
◽  
Puspraj Singh Puspraj Singh ◽  
Puspraj Singh Puspraj Singh ◽  
P. K. Chamadia P. K. Chamadia
Keyword(s):  
Magnetic Field ◽  
Solar Wind ◽  
Interplanetary Magnetic Field ◽  
Geomagnetic Storms ◽  
Radio Bursts ◽  
Solar Wind Disturbances

Radiometric Chronology of Neh–nar Glacier, Kashmir

1982 ◽  
Vol 28 (98) ◽  
pp. 91-105 ◽  
Author(s):  
V. N. Nijampurkar ◽  
N. Bhandari ◽  
C. P. Vohra ◽  
V. Krishnan
Keyword(s):  
Average Rate ◽  
Component Model ◽  
Vertical Profiles ◽  
Kashmir Valley ◽  
Movement Rate ◽  
Accumulation Zone ◽  
Core Samples ◽  
Surface Samples ◽  
Two Component

AbstractSurface and core samples of Neh–nar Glacier in the Kashmir Valley have been analysed for the radionuclides 32Si. 210Pb, 40K, and 137Cs. The lateral and vertical profiles (at an altitude of about 4 140 m) reveal:(1)32Si activity decreasing slowly from the accumulation zone to 4 050 m altitude and then abruptly towards the snout.(2)Five zones of alternating high and low 210Pb activity in the surface samples.(3)An horizon at between 2 and 3 m depth containing 210Pb activity above natural levels. This horizon is also associated with 137Cs and a maximum in total ß activity.The ice samples have been dated on the basis of a simplified two–component model, the “fresh“contribution determined by 2l0Pb and the old component by 32Si. The following conclusions can be drawn from these observations:(1)The model age of the snout ice is c. 850 years.(2)The average rate of ice movement in the lower glacier is about 2 m/year, which compares well with the annual movement rate of 2.65 m/year observed since 1974.

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