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DOI | 10.1038/s41586-019-1813-z |
Alfv茅nic velocity spikes and rotational flows in the near-Sun solar wind | |
J. C. Kasper; S. D. Bale; J. W. Belcher; M. Berthomier; A. W. Case; B. D. G. Chandran; D. W. Curtis; D. Gallagher; S. P. Gary; L. Golub; J. S. Halekas; G. C. Ho; T. S. Horbury; Q. Hu; J. Huang; K. G. Klein; K. E. Korreck; D. E. Larson; R. Livi; B. Maruca; B. Lavraud; P. Louarn; M. Maksimovic; M. Martinovic; D. McGinnis; N. V. Pogorelov; J. D. Richardson; R. M. Skoug; J. T. Steinberg; M. L. Stevens; A. Szabo; M. Velli; P. L. Whittlesey; K. H. Wright; G. P. Zank; R. J. MacDowall; D. J. McComas; R. L. McNutt Jr; M. Pulupa; N. E. Raouafi; N. A. Schwadron | |
2019-12-04 | |
发表期刊 | Nature
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出版年 | 2019 |
卷号 | 576页码:228-231 |
文章类型 | Article |
语种 | 英语 |
英文摘要 | The prediction of a supersonic solar wind1 was first confirmed by spacecraft near Earth2,3 and later by spacecraft at heliocentric distances as small as 62 solar radii4. These missions showed that plasma accelerates as it emerges from the corona, aided by unidentified processes that transport energy outwards from the Sun before depositing it in the wind. Alfv茅nic fluctuations are a promising candidate for such a process because they are seen in the corona and solar wind and contain considerable energy5,6,7. Magnetic tension forces the corona to co-rotate with the Sun, but any residual rotation far from the Sun reported until now has been much smaller than the amplitude of waves and deflections from interacting wind streams8. Here we report observations of solar-wind plasma at heliocentric distances of about 35 solar radii9,10,11, well within the distance at which stream interactions become important. We find that Alfv茅n waves organize into structured velocity spikes with duration of up to minutes, which are associated with propagating S-like bends in the magnetic-field lines. We detect an increasing rotational component to the聽flow velocity of the solar wind around the Sun, peaking at 35 to 50 kilometres per second鈥攃onsiderably above the amplitude of the waves. These flows exceed classical velocity predictions of a few kilometres per second, challenging models of circulation in the corona and calling into question our understanding of how stars lose angular momentum and spin down as they age12,13,14. |
领域 | 地球科学 ; 气候变化 ; 资源环境 |
URL | 查看原文 |
引用统计 | |
文献类型 | 期刊论文 |
条目标识符 | http://119.78.100.173/C666/handle/2XK7JSWQ/231900 |
专题 | 地球科学 资源环境科学 气候变化 |
推荐引用方式 GB/T 7714 | J. C. Kasper,S. D. Bale,J. W. Belcher,等. Alfv茅nic velocity spikes and rotational flows in the near-Sun solar wind[J]. Nature,2019,576:228-231. |
APA | J. C. Kasper.,S. D. Bale.,J. W. Belcher.,M. Berthomier.,A. W. Case.,...&N. A. Schwadron.(2019).Alfv茅nic velocity spikes and rotational flows in the near-Sun solar wind.Nature,576,228-231. |
MLA | J. C. Kasper,et al."Alfv茅nic velocity spikes and rotational flows in the near-Sun solar wind".Nature 576(2019):228-231. |
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