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

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).

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.

Quantum chaos and statistical properties of energy levels for atom in parallel electric and magnetic fields

2015 ◽  
Vol 29 (35n36) ◽  
pp. 1550248
Author(s):  
Hai-Feng Yang ◽  
Yong-Gang Tan ◽  
Zhong-Li Liu ◽  
Hong-Zhi Fu
Keyword(s):  
Magnetic Fields ◽  
Quantum Chaos ◽  
Chaotic Dynamics ◽  
Nearest Neighbor ◽  
Energy Levels ◽  
Statistical Properties ◽  
The Core ◽  
Ideal System ◽  
Electric And Magnetic Fields ◽  
Diagonalization Method

In this paper, the statistical properties of energy levels are studied numerically for atom in parallel electric and magnetic fields, which is an ideal system to examine the contributions of external fields and ionic core to quantum chaos. The Stark maps of diamagnetic spectra and nearest neighbor spacing (NNS) distributions are obtained by diagonalization method incorporating core effect. We identify obvious level anti-crossing and large value of [Formula: see text] for barium, indicating that core effect has predominant contribution to chaotic dynamics in barium. To study the core effect in detail, we sweep the quantum defect artificially and find that larger core effect will undoubtedly induce stronger chaotic dynamics.

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

scholarly journals Magnetic fields in the early Universe

2008 ◽  
Vol 4 (S259) ◽  
pp. 529-538 ◽  
Author(s):  
Eduardo Battaner ◽  
Estrella Florido
Keyword(s):  
Phase Transitions ◽  
Magnetic Fields ◽  
Early Universe ◽  
Galaxy Formation ◽  
Faraday Rotation ◽  
Large Scale ◽  
Large Scale Structure ◽  
Anisotropy Spectra ◽  
The Universe ◽  
Negligible Influence

AbstractThere is increasing evidence that intense magnetic fields exist at large redshifts. They could arise after galaxy formation or in very early processes, such as inflation or cosmological phase transitions, or both. Early co-moving magnetic strengths in the range 1-10 nG could be present at recombination. The possibilities to detect them in future CMB experiments are discussed, mainly considering their impact in the anisotropy spectra as a result of Faraday rotation and Alfven waves. Magnetic fields this magnitude could also have a non-negligible influence in determining the filamentary large scale structure of the Universe.

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