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Observations of Reconnection Flows in a Flare on the Solar Disk

  • Authors: Juntao Wang, P. J. A. Simões, N. L. S. Jeffrey, L. Fletcher, P. J. Wright, and I. G. Hannah

2017 The Astrophysical Journal Letters 847 L1.

  • Provider: AAS Journals

Caption: Figure 4.

Longitudinal velocity profiles for Fe XII and Fe XIII along the dotted line in Figure 3. The origin of the X axis represents the bottom of the dotted line. The dashed line is the linear fit for each profile. “b” represents the slope of the fit and its ﹩1-\sigma ﹩ uncertainty. The uncertainty for the rest wavelength estimation is ﹩\sim 5\,\mathrm{km}\,{{\rm{s}}}^{-1}﹩ for both lines, which would shift the entire profiles up or down.

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