The influence of a magnetic field, parallel to the cathode, on the second cathode sheath of a low-pressure arc discharge

1964 ◽  
Vol 11 (1) ◽  
pp. 418-422
Author(s):  
N. Warmoltz
Keyword(s):  
Magnetic Field ◽  
Arc Discharge ◽  
Low Pressure ◽  
Cathode Sheath ◽  
Field Parallel

Influence of magnetic field parallel to the arc on the formation of carbon nano-materials by arc discharge in water

Carbon ◽  
2009 ◽  
Vol 47 (8) ◽  
pp. 2131-2133 ◽  
Author(s):  
Gang Xing ◽  
Shenli Jia ◽  
Zongqian Shi
Keyword(s):  
Magnetic Field ◽  
Arc Discharge ◽  
Nano Materials ◽  
Field Parallel

Study of ionization processes in a low-pressure arc discharge

2019 ◽  
Vol 0 (9) ◽  
pp. 9-14
Author(s):  
A. V. Ushakov ◽  
◽  
I. V. Karpov ◽  
L. Yu. Fedorov ◽  
E.A. Dorozhkina ◽  
...  
Keyword(s):  
Arc Discharge ◽  
Low Pressure ◽  
Ionization Processes

Polarimetric and photometric observations of CB54, with analysis of four other dark clouds

2021 ◽  
Vol 503 (4) ◽  
pp. 5274-5290
Author(s):  
A K Sen ◽  
V B Il’in ◽  
M S Prokopjeva ◽  
R Gupta
Keyword(s):  
Magnetic Field ◽  
Near Infrared ◽  
Galactic Plane ◽  
Photometric Data ◽  
Dust Particles ◽  
Dark Cloud ◽  
Dark Clouds ◽  
High Polarization ◽  
Field Parallel ◽  
Photometric Observations

ABSTRACT We present the results of our BVR-band photometric and R-band polarimetric observations of ∼40 stars in the periphery of the dark cloud CB54. From different photometric data, we estimate E(B − V) and E(J − H). After involving data from other sources, we discuss the extinction variations towards CB54. We reveal two main dust layers: a foreground, E(B − V) ≈ 0.1 mag, at ∼200 pc and an extended layer, $E(B-V) \gtrsim 0.3$ mag, at ∼1.5 kpc. CB54 belongs to the latter. Based on these results, we consider the reason for the random polarization map that we have observed for CB54. We find that the foreground is characterized by low polarization ($P \lesssim 0.5$ per cent) and a magnetic field parallel to the Galactic plane. The extended layer shows high polarization (P up to 5–7 per cent). We suggest that the field in this layer is nearly perpendicular to the Galactic plane and both layers are essentially inhomogeneous. This allows us to explain the randomness of polarization vectors around CB54 generally. The data – primarily observed by us in this work for CB54, by A. K. Sen and colleagues in previous works for three dark clouds CB3, CB25 and CB39, and by other authors for a region including the B1 cloud – are analysed to explore any correlation between polarization, the near-infrared, E(J − H), and optical, E(B − V), excesses, and the distance to the background stars. If polarization and extinction are caused by the same set of dust particles, we should expect good correlations. However, we find that, for all the clouds, the correlations are not strong.

Magnetoresistance of a weakly disordered III-V semiconductor quantum well in a magnetic field parallel to interfaces

1997 ◽  
Vol 56 (11) ◽  
pp. 6436-6439 ◽  
Author(s):  
A. G. Mal’shukov ◽  
K. A. Chao ◽  
M. Willander
Keyword(s):  
Magnetic Field ◽  
Quantum Well ◽  
Field Parallel ◽  
Semiconductor Quantum Well
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