Anatomy of a Slow Wave in a Coronal Loop

Details Anatomy of a Slow Wave in a Coronal Loop Anatomy of a Slow Wave in a Coronal Loop

May 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010aas...21640708v&link_type=abstract

American Astronomical Society, AAS Meeting #216, #407.08; Bulletin of the American Astronomical Society, Vol. 41, p.860

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Scientific paper

We analyse an observation of a 5 minute quasi-periodic oscillation detected in the coronal line FeXII at 195A, near the footpoint of a coronal loop in Hinode/EIS data on 08 Feb 2007. The same oscillation is detected simultaneously in two other coronal lines, FeXIII at 204A and FeXI at 192A. The oscillation is observed for a full 2 periods in both Doppler shift and intensity. We use Fourier and wavelet analysis to determine the period of the oscillation to be P = 314 ± 83s in the Doppler shift and P = 344 ± 61s in the intensity. We observe negligible phase shift between Doppler and intensity time series. This is strong evidence for the interpretation of the observed phenomenon in terms of a propagating slow magneto-acoustic MHD mode. For the first time, we use spectroscopy to detect oscillations in the electron density, using the CHIANTI atomic database. Comparing the density variations and the Doppler shifts allows us to derive the line-of-sight component of the phase speed. The comparison of the temperature and the density allows to estimate the coronal value of the ratio of specific heats.
A comparative study of Hinode/EIS and multi-temperature high cadence SDO/AIA observations of this phenomenon is discussed.
The research leading to these results has received funding from the European community's seventh framework programme (FP7/2007-2013) under grant agreement number 220555.

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