Highly structured slow solar wind emerging from an equatorial coronal hole

@article{Bale2019HighlySS,
  title={Highly structured slow solar wind emerging from an equatorial coronal hole},
  author={Stuart. D. Bale and Samuel T. Badman and J. W. Bonnell and Trevor A. Bowen and David Burgess and Anthony William Case and Cynthia A. Cattell and Benjamin D. G. Chandran and Christopher C. Chaston and C. H. K. Chen and James F. Drake and Thierry Dudok de Wit and Jonathan P. Eastwood and Robert E. Ergun and William M. Farrell and C. Fong and Keith Goetz and Melvyn L. Goldstein and Katherine Amanda Goodrich and Peter R. Harvey and Timothy S. Horbury and Gregory Gershom Howes and Justin C. Kasper and Paul J. Kellogg and James A. Klimchuk and Kelly E. Korreck and Vladimir Krasnoselskikh and S{\"a}m Krucker and Ronan Laker and Davin E. Larson and Robert J. Macdowall and Milan Maksimovi{\'c} and David M. Malaspina and Juan Carlos Mart{\'i}nez-Oliveros and D. J. Mccomas and Nicole Meyer‐Vernet and Michel Moncuquet and Forrest S. Mozer and Tai D. Phan and Marc P. Pulupa and Noureddine Raouafi and Chadi S. Salem and David Stansby and Michael Louis Stevens and Adam Szabo and Marco Velli and Thomas Woolley and John R. Wygant},
  journal={Nature},
  year={2019},
  pages={1-6}
}
During the solar minimum, when the Sun is at its least active, the solar wind1,2 is observed at high latitudes as a predominantly fast (more than 500 kilometres per second), highly Alfvénic rarefied stream of plasma originating from deep within coronal holes. Closer to the ecliptic plane, the solar wind is interspersed with a more variable slow wind3 of less than 500 kilometres per second. The precise origins of the slow wind streams are less certain4; theories and observations suggest that… 
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