Resolving Azimuth Ambiguity Using Vertical Nature of Solar Quiet-Sun Magnetic Fields

@article{Gosain2013ResolvingAA,
  title={Resolving Azimuth Ambiguity Using Vertical Nature of Solar Quiet-Sun Magnetic Fields},
  author={Sanjay Gosain and Alexei A. Pevtsov},
  journal={Solar Physics},
  year={2013},
  volume={283},
  pages={195-205}
}
The measurement of solar magnetic fields using the Zeeman effect diagnostics has a fundamental 180° ambiguity in the determination of the azimuth angle of the transverse field component. There are several methods that are used in the community and each one has its merits and demerits. Here we present a disambiguation idea that is based on the assumption that most of the magnetic field on the sun is predominantly vertical. While the method is not applicable to penumbra or other features… 
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References

SHOWING 1-10 OF 16 REFERENCES
A New Technique for a Routine Azimuth Disambiguation of Solar Vector Magnetograms
We introduce a nonpotential magnetic field calculation (NPFC) technique to perform azimuth disambiguation in solar vector magnetograms. It is shown that resolving the 180° ambiguity would be a
A COMPARATIVE STUDY OF MAGNETIC FIELDS IN THE SOLAR PHOTOSPHERE AND CHROMOSPHERE AT EQUATORIAL AND POLAR LATITUDES
Besides their own intrinsic interest, correct interpretation of solar surface magnetic field observations is crucial to our ability to describe the global magnetic structure of the solar atmosphere.
An Overview of Existing Algorithms for Resolving the 180° Ambiguity in Vector Magnetic Fields: Quantitative Tests with Synthetic Data
We report here on the present state-of-the-art in algorithms used for resolving the 180° ambiguity in solar vector magnetic field measurements. With present observations and techniques, some
Studies of solar magnetic fields
AbstractSolar magnetic flux data accumulated from the magnetograph of the Mount Wilson Observatory are used to infer average east-west field inclination angles for the interval 1967–1973. In all
Transformation of vector magnetograms and the problems associated with the effects of perspective and the azimuthal ambiguity
Off-center vector magnetograms which use all three components of the measured field provide the maximum information content from the photospheric field and can provide the most consistent potential
Stokes profile analysis and vector magnetic fields. V: The magnetic field structure of large sunspots observed with Stokes II
Results are presented on the analysis of Stokes II polarimeter data on four large sunspots during 1980, yielding the vector magnetic field structure and thermodynamic parameters of these sunspots. It
East-west inclination of large-scale photospheric magnetic fields
Sixteen years of WSO magnetogram data have been studied to determine the solar cycle variation and latitude dependence of the east-west inclination of photospheric magnetic field lines. East-west
Studies of solar magnetic fields
An estimate of the average magnetic field strength at the poles of the Sun from Mount Wilson measurements is made by comparing low latitude magnetic measurements in the same regions made near the
Seething horizontal magnetic fields in the quiet solar photosphere
The photospheric magnetic field outside of active regions and the network has a ubiquitous and dynamic line-of-sight component that strengthens from disk center to limb as expected for a nearly
The Solar Optical Telescope for the Hinode Mission: An Overview
The Solar Optical Telescope (SOT) aboard the Hinode satellite (formerly called Solar-B) consists of the Optical Telescope Assembly (OTA) and the Focal Plane Package (FPP). The OTA is a 50-cm
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