Faraday Rotation Measurement of Trapped Magnetic Fields in a Thetapinch Plasma

1966 ◽  
Vol 9 (11) ◽  
pp. 2296 ◽  
Author(s):  
P. Bogen
Keyword(s):  
Magnetic Fields ◽  
Faraday Rotation ◽  
Rotation Measurement

scholarly journals Implementation of a Faraday rotation diagnostic at the OMEGA laser facility

2018 ◽  
Vol 6 ◽  
Author(s):  
A. Rigby ◽  
J. Katz ◽  
A. F. A. Bott ◽  
T. G. White ◽  
P. Tzeferacos ◽  
...  
Keyword(s):  
Magnetic Field ◽  
Magnetic Fields ◽  
Faraday Rotation ◽  
Field Measurements ◽  
Thomson Scattering ◽  
Proton Radiography ◽  
Time Resolved ◽  
Rotation Measurement ◽  
Laser Facility ◽  
Omega Laser

Magnetic field measurements in turbulent plasmas are often difficult to perform. Here we show that for ${\geqslant}$kG magnetic fields, a time-resolved Faraday rotation measurement can be made at the OMEGA laser facility. This diagnostic has been implemented using the Thomson scattering probe beam and the resultant path-integrated magnetic field has been compared with that of proton radiography. Accurate measurement of magnetic fields is essential for satisfying the scientific goals of many current laser–plasma experiments.

Magnetic fields in the intergalactic medium and in the cosmic web

2018 ◽  
Vol 14 (A30) ◽  
pp. 303-306
Author(s):  
Marcus Brüggen ◽  
Shane O’Sullivan ◽  
Annalisa Bonafede ◽  
Franco Vazza
Keyword(s):  
Magnetic Fields ◽  
Faraday Rotation ◽  
Large Scale ◽  
Intergalactic Medium ◽  
Angular Resolution ◽  
Low Frequency ◽  
Small Scale ◽  
Rotation Measurement ◽  
Field Amplification ◽  
Unique Capability

AbstractIn these proceedings we discuss advances in the theory and observation of magnetic fields in the intergalactic medium and in the cosmic web. We make the point that, despite perhaps unsurmountable obstacles in simulating a small-scale dynamo, currently most cosmological magnetohydrodynamical simulations paint a similar picture of magnetic field amplification in the cosmos. However, observations of magnetic fields in the intergalactic medium turn out to be very difficult. As a case in point, we present recent work on Faraday rotation measurement in the direction of a giant galaxy with the Low Frequency Array (LOFAR). These observations demonstrate the currently unique capability of LOFAR to measure Faraday rotation at the high accuracy and angular resolution required to investigate the magnetisation of large-scale structure filaments of the cosmic web.

scholarly journals An 84-μG Magnetic Field in a Galaxy at Z=0.692?

2008 ◽  
Vol 4 (S254) ◽  
pp. 95-96
Author(s):  
Arthur M. Wolfe ◽  
Regina A. Jorgenson ◽  
Timothy Robishaw ◽  
Carl Heiles ◽  
Jason X. Prochaska
Keyword(s):  
Magnetic Field ◽  
Magnetic Fields ◽  
Faraday Rotation ◽  
Large Scale ◽  
Dynamo Model ◽  
Magnetic Field Generation ◽  
Interstellar Gas ◽  
Splitting Technique ◽  
Average Value ◽  
The Magnetic Field

AbstractThe magnetic field pervading our Galaxy is a crucial constituent of the interstellar medium: it mediates the dynamics of interstellar clouds, the energy density of cosmic rays, and the formation of stars (Beck 2005). The field associated with ionized interstellar gas has been determined through observations of pulsars in our Galaxy. Radio-frequency measurements of pulse dispersion and the rotation of the plane of linear polarization, i.e., Faraday rotation, yield an average value B ≈ 3 μG (Han et al. 2006). The possible detection of Faraday rotation of linearly polarized photons emitted by high-redshift quasars (Kronberg et al. 2008) suggests similar magnetic fields are present in foreground galaxies with redshifts z > 1. As Faraday rotation alone, however, determines neither the magnitude nor the redshift of the magnetic field, the strength of galactic magnetic fields at redshifts z > 0 remains uncertain.Here we report a measurement of a magnetic field of B ≈ 84 μG in a galaxy at z =0.692, using the same Zeeman-splitting technique that revealed an average value of B = 6 μG in the neutral interstellar gas of our Galaxy (Heiles et al. 2004). This is unexpected, as the leading theory of magnetic field generation, the mean-field dynamo model, predicts large-scale magnetic fields to be weaker in the past, rather than stronger (Parker 1970).The full text of this paper was published in Nature (Wolfe et al. 2008).

Observation of the nearest-neighbor magnetization step in CdS:Co by Faraday rotation in magnetic fields to 60 T

1995 ◽  
Vol 51 (24) ◽  
pp. 17561-17564 ◽  
Author(s):  
M. Dahl ◽  
D. Heiman ◽  
S. Foner ◽  
T. Q. Vu ◽  
R. Kershaw ◽  
...  
Keyword(s):  
Magnetic Fields ◽  
Faraday Rotation ◽  
Nearest Neighbor

Dual-channel Faraday rotation measurement for pulsed magnetic field

2021 ◽  
Vol 92 (10) ◽  
pp. 105004
Author(s):  
Jue Zhang ◽  
Xincai Zhao ◽  
Guanghua Chen ◽  
Qixian Peng
Keyword(s):  
Magnetic Field ◽  
Faraday Rotation ◽  
Pulsed Magnetic Field ◽  
Rotation Measurement ◽  
Dual Channel

Faraday rotation measurement with photorefractive Bi12TiO20: comment

2003 ◽  
Vol 35 (4) ◽  
pp. 319
Author(s):  
Eugenio Garbusi ◽  
José A. Ferrari
Keyword(s):  
Faraday Rotation ◽  
Rotation Measurement

scholarly journals Could bow-shaped magnetic morphologies surround filamentary molecular clouds?

2019 ◽  
Vol 632 ◽  
pp. A68 ◽  
Author(s):  
M. Tahani ◽  
R. Plume ◽  
J. C. Brown ◽  
J. D. Soler ◽  
J. Kainulainen
Keyword(s):  
Magnetic Field ◽  
Monte Carlo ◽  
Magnetic Fields ◽  
Faraday Rotation ◽  
Molecular Clouds ◽  
Monte Carlo Analysis ◽  
Line Of Sight ◽  
Field Reversal ◽  
Filamentary Structure ◽  
Western Side

Context. A new method based on Faraday rotation measurements recently found the line-of-sight component of magnetic fields in Orion-A and showed that their direction changes from the eastern side of this filamentary structure to its western side. Three possible magnetic field morphologies that can explain this reversal across the Orion-A region are toroidal, helical, and bow-shaped morphologies. Aims. In this paper, we constructed simple models to represent these three morphologies and compared them with the available observational data to find the most probable morphology(ies). Methods. We compared the observations with the models and used probability values and a Monte Carlo analysis to determine the most likely magnetic field morphology among these three morphologies. Results. We found that the bow morphology had the highest probability values, and that our Monte-Carlo analysis suggested that the bow morphology was more likely. Conclusions. We suggest that the bow morphology is the most likely and the most natural of the three morphologies that could explain a magnetic field reversal across the Orion-A filamentary structure (i.e., bow, helical and toroidal morphologies).

scholarly journals DENSER SAMPLING OF THE ROSETTE NEBULA WITH FARADAY ROTATION MEASUREMENTS: IMPROVED ESTIMATES OF MAGNETIC FIELDS IN H ii REGIONS

2016 ◽  
Vol 821 (2) ◽  
pp. 92 ◽  
Author(s):  
Allison H. Costa ◽  
Steven R. Spangler ◽  
Joseph R. Sink ◽  
Shea Brown ◽  
Sui Ann Mao
Keyword(s):  
Magnetic Fields ◽  
Faraday Rotation ◽  
H Ii Regions ◽  
Rosette Nebula

Time-dependent effects in Faraday rotation in pulsed magnetic fields: an explanation

1985 ◽  
Vol 24 (12) ◽  
pp. 1780 ◽  
Author(s):  
Jeffrey A. Davis ◽  
M. Azad Islam ◽  
Roger A. Lilly
Keyword(s):  
Magnetic Fields ◽  
Faraday Rotation ◽  
Time Dependent ◽  
Pulsed Magnetic Fields
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