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- W2028483642 endingPage "288" @default.
- W2028483642 startingPage "267" @default.
- W2028483642 abstract "Coronal holes are the coolest and darkest regions of the upper solar atmosphere, as observed both on the solar disk and above the solar limb. Coronal holes are associated with rapidly expanding open magnetic fields and the acceleration of the high-speed solar wind. During the years of the solar minima, coronal holes are generally confined to the Sun’s polar regions, while at solar maxima they can also be found at lower latitudes. Waves, observed via remote sensing and detected in-situ in the wind streams, are most likely responsible for the wind and several theoretical models describe the role of MHD waves in the acceleration of the fast solar wind. This paper reviews the observational evidences of detection of propagating waves in these regions. The characteristics of the waves, like periodicities, amplitude, speed provide input parameters and also act as constraints on theoretical models of coronal heating and solar wind acceleration." @default.
- W2028483642 created "2016-06-24" @default.
- W2028483642 creator A5021267276 @default.
- W2028483642 creator A5027573957 @default.
- W2028483642 creator A5060583589 @default.
- W2028483642 date "2010-11-03" @default.
- W2028483642 modified "2023-10-16" @default.
- W2028483642 title "Propagating MHD Waves in Coronal Holes" @default.
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