Faraday Rotation Dispersion Microscopy Imaging of Diamagnetic and Chiral Liquids with Pulsed Magnetic Field

2013 ◽  
Vol 85 (10) ◽  
pp. 5176-5183 ◽  
Author(s):  
Masayori Suwa ◽  
Yusuke Nakano ◽  
Satoshi Tsukahara ◽  
Hitoshi Watarai
Keyword(s):  
Magnetic Field ◽  
Faraday Rotation ◽  
Pulsed Magnetic Field ◽  
Microscopy Imaging ◽  
Rotation Dispersion

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

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).

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