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Intermittent Reconnection and Plasmoids in UV Bursts in the Low Solar Atmosphere

  • Authors: L. Rouppe van der Voort, B. De Pontieu, G. B. Scharmer, J. de la Cruz Rodríguez, J. Martínez-Sykora, D. Nóbrega-Siverio, L. J. Guo, S. Jafarzadeh, T. M. D. Pereira, V. H. Hansteen, M. Carlsson, and G. Vissers

2017 The Astrophysical Journal Letters 851 L6.

  • Provider: AAS Journals

Caption: Figure 4.

Results from the Bifrost simulation. Synthetic spectral profiles of Si IV (a) and Ca II (b) computed along the inclined line shown in panels (d)–(h), which crosses some plasmoids. Panel (c) shows the spacetime plot of Ca II blue wing (25 km s−1) with the LOS along the vertical axis. The red horizontal line is marking the time of the other panels. Maps of the density, velocity along the inclined LOS, and temperature are shown in panels (e), (f), and (g). The white contours in panel (g) mark the heights of ﹩\tau =0.3,1,3﹩ along the vertical LOS for the −25 km s−1 blue wing of Ca II K. Panels (d) and (h) show the absolute magnitude of the magnetic field, with (d) zooming in on plasmoids that can be recognized as magnetic islands by selected field lines (white contours). The plasmoids are readily seen in the density map and correspond to very narrow Ca II brightenings that travel from left to right in panel (c) and are highlighted by ellipses: the red ellipse marks the plasmoids that produced the Ca II K profile in panel (b), the orange ellipses mark earlier episodes with plasmoids visible in the Ca II K blue wing. Colored markers in panel (e) indicate the location of ﹩\tau =1﹩ of the corresponding Ca II K spectral features in panel (b); the peaks at ﹩-29,-16﹩, and −3 km s−1 (green, dark blue, and pink markers) are caused by different plasmoids. An animated version of panels (c), (e), (f), and (g) is available.

(An animation of this figure is available.)

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

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