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

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

2012-04-11

arxiv.org/abs/1204.2544v2

Astronomy and Astrophysics

Astrophysics

Solar and Stellar Astrophysics

Scientific paper

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 Alfv\'en waves off-limb in polar coronal hole up to $\simeq 0.4$ R$_\odot$. The computed Alfv\'en 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$^{-1}$. Hence, this result suggests energy deposition by Alfv\'en waves in a polar coronal hole, thus providing a significant source for coronal heating.

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