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MAGNETIC UPFLOW EVENTS IN THE QUIET-SUN PHOTOSPHERE. I. OBSERVATIONS

  • Authors: S. Jafarzadeh, L. Rouppe van der Voort, and J. de la Cruz Rodríguez

2015 The Astrophysical Journal 810 54.

  • Provider: AAS Journals

Caption: Figure 5.

Examples of different shapes (classes) of Stokes V profiles of the magnetic upflow events (MUEs): (Ia) asymmetric but clear double-lobed profile, (Ib) asymmetric with a weak second lobe, (II) largely asymmetric, single-lobed profile, (III) a profile with two same-polarity lobes, and (IV) double-lobed profile with an extra blueshifted bump. The bottom right panel represents a typical example of a normal (double-lobe, antisymmetric) profile of a non-MUE as a reference. Plotted in gray are the profiles corresponding to all individual pixels of the MUEs marked by the green circles on the right panels. The mean profiles (black lines) as well as the sampled wavelength positions (blue filled circles) are overlaid. The vertical lines mark the rest wavelengths of line cores of the 6301 and 6302 Å spectra. The red dash-dotted lines indicate the ﹩3\sigma ﹩ noise level of the corresponding averaged profiles. The right panels of the profiles show the images of far-blue-wing Stokes V (top), in-line Stokes V (middle), and continuum Stokes I (bottom), with side lengths of ﹩\approx 2﹩ arcsec. The in-line V images are saturated to the same scale as their corresponding far-blue-wing V images. The blue and red contours in the continuum images indicate the locations of MBEs and MREs in the field of view, respectively. The yellow cross in the bottom right panel marks a network pixel for which the reference profile is plotted.

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