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Inconspicuous Solar Polar Coronal X-Ray Jets as the Source of Conspicuous Hinode/EUV Imaging Spectrometer Doppler Outflows

  • Authors: Alphonse C. Sterling, Conrad Schwanitz, Louise K. Harra, Nour E. Raouafi, Navdeep K. Panesar, Ronald L. Moore

Alphonse C. Sterling et al 2022 The Astrophysical Journal 940 .

  • Provider: AAS Journals

Caption: Figure 6.

Zoomed-in views of Table 1 event 5, at AIA and XRT wavelengths. The basic layout of the panels is as described in Figure 3. Green arrows show a cool-material erupting minifilament, at about the same time in (a), (b), (d), and (e). Blue arrows in (i) and (l) show a brightening similar to a JBP, and that brightening is visible but saturated in the AIA images in (g), (h), (j), and (k). White arrows in (l) point to either side of a faint feature that resembles a coronal-jet spire. Blue lines in (k) and (l) represent portions of the EIS field of view (FOV) shown in Figure 1, and which is shown as a white box in the video accompanying Figure 2. The animation accompanying the current figure shows the evolution of these panels, covering 2020 March 7 over 17:47–18:44 UT. The animation runs twice, where the first time through an arrow in the 171 Å panel shows outflows from the minifilament-eruption location that reach out to the location near where the spire forms, and the blue lines in the XRT panel represent the FOV of the panel for event 5 in the animation accompanying Figure 1. The second time through the animation plays without the arrow and box overlays. The entire movie runs for 6 s. From Table 1 the center of the blueshift contour is at about 18:32 UT, at which time the XRT movie is still consistent with continued outflow.

(An animation of this figure is available.)

The video/animation of this figure is available in the online journal.

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