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DIRECT OBSERVATION OF SOLAR CORONAL MAGNETIC FIELDS BY VECTOR TOMOGRAPHY OF THE CORONAL EMISSION LINE POLARIZATIONS

  • Authors: M. Kramar, H. Lin, and S. Tomczyk

2016 The Astrophysical Journal Letters 819 L36.

  • Provider: AAS Journals

Caption: Figure 3.

Distributions of the angular differences between the tomography reconstructed magnetic field vectors and that of the MHD model used as the starting field of the tomographic inversion in regions A (green), B (dashed red), C (black), D (black dashed), and E (blue). The distributions are within ±10° in longitude and latitude from longitude and latitude of (20.°5; −40.°5) (region A), (30.°5; 46.°5) (B), (290.°5; 40.°5) (C), and (30.°5; −20.°5) (D). Region E covers the entire solid angle of ﹩4\pi ﹩. The distributions are within heliocentric distances of ﹩[1.05;1.25]﹩ (left) and ﹩[1.10;1.25]{R}_{\odot }﹩ (right).

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