Abstract
Large amplitude fluctuations, often with characteristics reminiscent of large amplitude Alfvén waves propagating away from the Sun, are ubiquitous in the solar wind. Such features are most frequently found within fast solar wind streams and most often at solar minimum. The fluctuations found in slow solar wind streams usually have a smaller relative amplitude, are less Alfvénic in character and present more variability. However, intervals of slow wind displaying Alfvénic correlations have been recently identified in different solar cycle phases. In the present paper we report Alfvénic slow solar wind streams seen during the maximum of solar activity that are characterized not only by a very high correlation between velocity and magnetic field fluctuations (as required by outwardly propagating Alfvén modes) – comparable to that seen in fast wind streams – but also by higher amplitude relative fluctuations comparable to those seen in fast wind. Our results suggest that the Alfvénic slow wind has a different origin from the slow wind found near the boundary of coronal holes, where the amplitude of the Alfvénic fluctuations decreases together with decreasing the wind speed.
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Acknowledgements
The authors are grateful to the following people and organizations for data provision: R. Lin (UC Berkeley) and R. P. Lepping (NASA/GSFC) for WIND/3DP and WIND/MFI data, respectively. All these data are available on the NASA-CDAWeb website: https://cdaweb.sci.gsfc.nasa.gov/index.html.
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Solar Wind at the Dawn of the Parker Solar Probe and Solar Orbiter Era
Guest Editors: Giovanni Lapenta and Andrei Zhukov
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D’Amicis, R., Matteini, L., Bruno, R. et al. Large Amplitude Fluctuations in the Alfvénic Solar Wind. Sol Phys 295, 46 (2020). https://doi.org/10.1007/s11207-020-01606-2
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DOI: https://doi.org/10.1007/s11207-020-01606-2