File:Coronal jet and surge.png
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Captions
Captions
Coronal jet and surge in a radiation-MHD numerical experiment by Nóbrega-Siverio et al. (2017, 2018)
Summary[edit]
| Description |
English: This figure shows a snapshot from a solar bidimensional radiation-magnetohydrodynamic (R-MHD) numerical experiment by Nóbrega-Siverio et al. (2017, 2018) carried out using the Bifrost code (Gudiksen et al. 2011). In the left panel, a temperature, T, map from that simulation is shown, spanning from the upper layers of the convection zone up to the solar corona, where the location of the solar surface is indicated with a dash line at Z=0 Mm. In that panel, we can distinguish a dome-like structure that corresponds to a new emerged plasma that has raised from the solar interior and that is now being reconnected with the pre-existing coronal magnetic field. As a consequence of this magnetic reconnection process, two ejections are produced: a hot collimated coronal jet with an inverted-Y shape (or Eiffel tower) that reaches more than 1 MK; and a non-collimated ejection with a fang shape, known as surge, composed by cool plasma. The middle panel contains a map of the vertical velocity, uz, for the same instant and domain illustrated in the left panel. This panel shows that the coronal jet reaches velocities of more 150 km/s, in fact, the upwards velocities are up to 300 km/s (the color scale is saturated), while the surge has downward velocities, as maximum, of -50 km/s. The right panel contains a zoom out for the previous panel to highlight the reconnection site and the bidirectionial flow that leads to the hot coronal jet.
Español: Esta figura muestra una instantánea de un experimento numérico solar bidimensional radiativo-magnetohidrodinámico (R-MHD) de Nóbrega-Siverio et al. (2017, 2018) llevado a cabo utilizando el código Bifrost (Gudiksen et al. 2011). En el panel izquierdo, se muestra un mapa de temperatura, T, de esa simulación, que abarca desde las capas superiores de la zona de convección hasta la corona solar, donde la localización de la superficie solar está indicada co una línea discontinua en Z=0 Mm. En dicho panel podemos distinguir una estructura tipo cúpula que corresponde a nuevo plasma emergente que se ha elevado desde el interior solar y que ahora se está reconectando con el campo magnético coronal preexistente. Como consecuencia de este proceso de reconexión magnética, se producen dos eyecciones: un jet coronal colimado y caliente con forma de Y invertida (o torre Eiffel) que alcanza más de 1 MK; y una eyección no colimada con forma de colmillo, conocida como surge, compuesta por plasma frío. El panel central contiene un mapa de la velocidad vertical, uz, para el mismo instante temporal y dominio ilustrado en el panel izquierdo. Este panel muestra que el jet coronal alcanza velocidades de más de 150 km/s, de hecho, las velocidades ascendentes son de hasta 300 km/s (la escala de colores está saturada), mientras que el surge tiene velocidades descendentes de, como máximo, -50 km / s. El panel derecho contiene un zoom del panel anterior para resaltar el sitio de reconexión y el flujo bidireccional que conduce al jet coronal caliente. |
| Date | |
| Source | Own work |
| Author | Daniel Nóbrega-Siverio |
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| Date/Time | Thumbnail | Dimensions | User | Comment | |
|---|---|---|---|---|---|
| current | 21:28, 23 February 2020 | | 3,009 × 1,740 (1.29 MB) | Desiveri (talk | contribs) | User created page with UploadWizard |
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