On the parallel and perpendicular propagating motions visible in polar plumes: an incubator for (fast) solar wind acceleration?

Jiajia Liu*, Scott W. McIntosh, Ineke De Moortel, Yuming Wang

*Corresponding author for this work

Research output: Contribution to journalArticlepeer-review

10 Citations (Scopus)
1 Downloads (Pure)

Abstract

We combine observations of the Coronal Multi-channel Polarimeter and the Atmospheric Imaging Assembly on board the Solar Dynamics Observatory 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(-1) (in both the 171 and 193 angstrom passbands) and a periodicity of 15 minutes, while the (perpendicular) Alfvenic wave motions have a velocity amplitude of 0.5 km s(-1), a phase speed of 830 km s(-1), 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.

Original languageEnglish
Article number273
Number of pages7
JournalAstrophysical Journal
Volume806
Issue number2
DOIs
Publication statusPublished - 20 Jun 2015

Keywords

  • Sun: corona
  • Waves
  • Coronal loops
  • Alfven waves
  • Turbulance-driven
  • Energy content
  • Chromosphere
  • Holes
  • Macrospicules
  • Oscillations
  • Seismology
  • Region

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