期刊
ASTROPHYSICAL JOURNAL
卷 759, 期 1, 页码 -出版社
IOP PUBLISHING LTD
DOI: 10.1088/0004-637X/759/1/33
关键词
magnetic reconnection; plasmas; Sun: activity; Sun: chromosphere; Sun: magnetic topology
资金
- Ministry of Education, Culture, Sports, Science, and Technology (MEXT) of Japan
- Science and Technology Facilities Council [ST/H000429/1, PP/D002907/1] Funding Source: researchfish
- UK Space Agency [ST/J001732/1] Funding Source: researchfish
- Grants-in-Aid for Scientific Research [24740132] Funding Source: KAKEN
- STFC [ST/H000429/1, PP/D002907/1] Funding Source: UKRI
The recent discovery of chromospheric anemone jets with the Solar Optical Telescope (SOT) on board Hinode has shown an indirect evidence of magnetic reconnection in the solar chromosphere. However, the basic nature of magnetic reconnection in chromosphere is still unclear. We studied nine chromospheric anemone jets from SOT/ Hinode using Ca II H filtergrams, and we found multiple bright, plasma ejections along the jets. In most cases, the major intensity enhancements (larger than 30% relative to the background intensity) of the loop correspond to the timing of the plasma ejections. The typical lifetime and size of the plasma ejecta are about 20-60 s and 0.3-1.5 Mm, respectively. The height-time plot of jet shows many sub-structures (or individual jets) and the typical lifetime of the individual jet is about one to five minutes. Before the onset of the jet activity, a loop appears in Ca II H and gradually increases in size, and after few minutes several jets are launched from the loop. Once the jet activity starts and several individual jets are launched, the loop starts shrinking with a speed of similar to 4 km s(-1). In some events, a downward moving blob with a speed of similar to 35 km s(-1) was observed, associated with the upward moving plasma along one of the legs of the loop hosting the jets. The upward moving plasma gradually developed into jets. Multiple plasma ejections in chromospheric anemone jet show the strongly time-dependent as well as intermittent nature of magnetic reconnection in the solar chromosphere.
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