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TEMPORAL EVOLUTION OF MULTIPLE EVAPORATING RIBBON SOURCES IN A SOLAR FLARE

  • Authors: D. R. Graham, and G. Cauzzi

2015 The Astrophysical Journal Letters 807 L22.

  • Provider: AAS Journals

Caption: Figure 2.

Left panels: fits of the Fe XXI 1354.1 Å line (green) for slit position y = 122″. The observed spectrum is shown by the stepped black line, with the total fit in black on top; cooler components are shown by a dotted line. The non-thermal FWHM, vnt, is also shown. Right panels: Mg II subordinate line with bisector positions at 10% intensity increments marked by black squares, and the rest wavelength (2791.56 Å) by the vertical dashed line.

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