On the Parallel and Perpendicular Propagating Motions Visible in Polar Plumes: An Incubator For (Fast) Solar Wind Acceleration?

Abstract

We combine observations of the Coronal Multi-channel Polarimeter (CoMP) and the Atmospheric Imaging Assembly (AIA) onboard the Solar Dynamics Observatory (SDO) to study the characteristic properties of (propagating) Alfvenic motions and quasi-periodic intensity disturbances in polar plumes. This unique combination of instruments highlights the physical richness of the processes taking place at the base of the (fast) solar wind. The (parallel) intensity perturbations with intensity enhancements around 1% have an apparent speed of 120 km/s (in both the 171A and 193A passbands) and a periodicity of 15 minutes, while the (perpendicular) Alfvenic wave motions have a velocity amplitude of 0.5 km/s, a phase speed of 830 km/s, and a shorter period of 5 minutes on the same structures. These observations illustrate a scenario where the excited Alfvenic motions are propagating along an inhomogeneously loaded magnetic field structure such that the combination could be a potential progenitor of the magnetohydrodynamic turbulence required to accelerate the fast solar wind.

15 pages, 4 figures and 1 table

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• Observing the Roots of Solar Coronal Heating - in the Chromosphere
• The Spectroscopic Signature of Quasi-periodic Upflows in Active Region Timeseries
• STEREO Observations of Quasi-Periodically Driven High Velocity Outflows in Polar Plumes
• Propagating waves in polar coronal holes as seen by SUMER and EIS
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• Statistical properties of Hα jets in the polar coronal hole and their implications in coronal activities
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• A new facility for airborne solar astronomy: NASA's WB-57 at the 2017 total solar eclipse