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: http://star.arm.ac.uk/highlights/2014/658.html
Дата изменения: Thu Oct 23 18:08:46 2014 Дата индексирования: Sun Apr 10 02:56:36 2016 Кодировка: Поисковые слова: р п р п р п р п р п р п р п р п р п р п р п р п р п р п р п р п р п р п р п р п р п р п |
The detection of upwardly propagating waves channelling energy from the chromosphere to the low corona
Figure 1. The region of plasma analysed in this article sampled at 07 : 23 UT: An overview of the field-of-view (FOV) inferred by SST/CRISP and SDO/AIA consisting of: (a) SDO/AIA 170 nm, detailing the photosphere; (b) SST Hα 656.28 nm (line core) sampling the chromosphere; the (c) SDO/AIA 30.4 nm filter (TR); and the lower corona detailed by (d) SDO/AIA 17.1 nm. The white line on each image represents the slit used to construct the time-distance diagrams plotted in Fig. 3. The cyan lines outline each slit used to investigate UPW behaviour.
Abstract
Understanding how the multi-million kelvin corona is heated to such extreme temperatures has so far proved difficult. Numerous mechanisms, including magnetohydrodynamic (MHD) waves have been suggested which could provide an explanation; however, no observations have yet tracked the direct propagation of a wave train from the lower into the upper solar atmosphere. Here, we present the first observation of wave-based energy transport from the chromosphere to the transition region (TR) and corona by upwardly propagating waves (UPWs) around a large magnetic field concentration. We propose that the amount of energy potentially deposited into the corona above active regions (ARs) by these waves could offer a realistic answer to the important question of how the corona is energised.
Last Revised: 2014 October 23rd |