Chitta L P, Zhukov A N, Berghmans D, Peter H, Parenti S, Mandal S, Aznar Cuadrado R, Schühle U, Teriaca L, Auchère F, Barczynski K, Buchlin É, Harra L, Kraaikamp E, Long D M, Rodriguez L, Schwanitz C, Smith P J, Verbeeck C, Seaton D B
Max-Planck-Institut für Sonnensystemforschung, 37077 Göttingen, Germany.
Solar-Terrestrial Centre of Excellence, Solar Influences Data Analysis Centre, Royal Observatory of Belgium, 1180 Brussels, Belgium.
Science. 2023 Aug 25;381(6660):867-872. doi: 10.1126/science.ade5801. Epub 2023 Aug 24.
Coronal holes are areas on the Sun with open magnetic field lines. They are a source region of the solar wind, but how the wind emerges from coronal holes is not known. We observed a coronal hole using the Extreme Ultraviolet Imager on the Solar Orbiter spacecraft. We identified jets on scales of a few hundred kilometers, which last 20 to 100 seconds and reach speeds of ~100 kilometers per second. The jets are powered by magnetic reconnection and have kinetic energy in the picoflare range. They are intermittent but widespread within the observed coronal hole. We suggest that such picoflare jets could produce enough high-temperature plasma to sustain the solar wind and that the wind emerges from coronal holes as a highly intermittent outflow at small scales.
冕洞是太阳上具有开放磁力线的区域。它们是太阳风的一个源区，但太阳风如何从冕洞出现尚不清楚。我们使用太阳轨道飞行器上的极紫外成像仪观测了一个冕洞。我们识别出了几百公里尺度的喷流，其持续20到100秒，速度达到约每秒100公里。这些喷流由磁重联提供能量，具有皮耀斑范围内的动能。它们是间歇性的，但在观测到的冕洞内广泛存在。我们认为，这样的皮耀斑喷流能够产生足够的高温等离子体来维持太阳风，并且太阳风以小尺度上高度间歇性的外流形式从冕洞出现。
