Spectroscopic signature of Alfvén waves damping in a polar coronal hole up to 0.4 solar radii

Abstract

Between February 24-25, 2009, the EIS spectrometer onboard the Hinode spacecraft performed special "sit & stare" observations above the South polar coronal hole continuously over more than 22 hours. Spectra were acquired with the 1" slit placed off-limb covering altitudes up to 0.48 R${}_{\odot }$ ($3.34\times 10^2$ Mm) above the Sun surface, in order to study with EIS the non-thermal spectral line broadenings. Spectral lines such as Fe {\sc xii} $\lambda$186.88, Fe {\sc xii} $\lambda$193.51, Fe {\sc xii} $\lambda$195.12 and Fe {\sc xiii} $\lambda$202.04 are observed with good statistics up to high altitudes and they have been analyzed in this study. Results show that the FWHM of Fe {\sc xii} $\lambda$195.12 line increases up to $\simeq 0.14$ R${}_{\odot }$, then decreases higher up. EIS stray light has been estimated and removed. Derived electron density and non-thermal velocity profiles have been used to estimate the total energy flux transported by Alfvén waves off-limb in polar coronal hole up to $\simeq 0.4$ R${}_{\odot }$. The computed Alfvén wave energy flux density $f_w$ progressively decays with altitude from $f_w\simeq 1.2\cdot 10^6$ erg cm${}^{-2}$ s${}^{-1}$ at 0.03 R${}_{\odot }$ down to $f_w\simeq 8.5\cdot 10^3$ erg cm${}^{-2}$ s${}^{-1}$ at 0.4 R${}_{\odot }$, with an average energy decay rate $\Delta f_w/\Delta h\simeq -4.5\cdot 10^{-5}$ erg cm${}^{-3}$ s${}^{-1}$. Hence, this result suggests energy deposition by Alfvén waves in a polar coronal hole, thus providing a significant source for coronal heating.

Physical units of the Alfvén wave Energy Decay Rate $\Delta f_w/\Delta h$ revised with respect to the published version. Scientific results and conclusions unchanged

References in corpus (5)

• High precision density measurements in the solar corona: I. Analysis methods and results for Fe XII and Fe XIII
• Modelling of EIS spectrum drift from instrumental temperatures
• Accelerating waves in polar coronal holes as seen by EIS and SUMER
• Solar off-limb line widths: Alfven waves, ion-cyclotron waves, and preferential heating
• Spectral line width decrease in the solar corona: resonant energy conversion from Alfv{é}n to acoustic waves

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